HELIO HEC Lists

List IDList Name
aad_gleAAD Ground Level Enhancement List
cactus_soho_cmeCACTus SOHO/LASCO CME List
cactus_soho_flowCACTus SOHO/LASCO Flow List
cactus_stereoa_cmeCACTus STEREO-A/COR CME List
cactus_stereoa_flowCACTus STEREO-A/COR Flow List
cactus_stereob_cmeCACTus STEREO-B/COR CME List
cactus_stereob_flowCACTus STEREO-B/COR Flow List
stereo_impactplastic_icmeCatalogue of Interplanetary Coronal Mass Ejections from STEREO IMPACT/PLASTIC
stereoa_impactplastic_shockcatalogue of Interplanetary Shocks from STEREO-A IMPACT/PLASTIC
stereob_impactplastic_shockCatalogue of Interplanetary Shocks from STEREO-B IMPACT/PLASTIC
stereoa_impactplastic_sirCatalogue of Stream Interaction Regions (SIRs) from STEREO-A IMPACT/PLASTIC
stereob_impactplastic_sirCatalogue of Stream Interaction Regions (SIRs) from STEREO-B IMPACT/PLASTIC
cme_forbush_eventCME-related Forbush Decrease Event List
cme_inner_heliosphereCMEs in the Inner Heliosphere
goes_proton_eventGOES Proton Event List
goes_sxr_flareGOES Soft X-ray Flare List
goes_flare_sep_eventGOES Strong Flares and associated SEP Events
istp_sw_eventISTP Solar Wind Candidate Event List
kso_halpha_flareKanzelhoehe Solar Observatory (KSO) H-alpha Flare List
goes_flare_no_sep_radio_cmeList of Radio and CME associations for GOES flares without SEP
mars_earth_icmeMars Earth ICME List
icme_earth_cycle23Near-Earth Interplanetary Coronal Mass Ejections During Solar Cycle 23
ngdc_aastar_stormNGDC AA* Major Magnetic Storm List
ngdc_apstar_stormNGDC Ap* Major Magnetic Storm List
ngdc_halpha_flareNGDC H-alpha Flare List
ngdc_sscNGDC Storm Sudden Commencement List
noaa_energetic_eventNOAA Solar Energetic Event List
noaa_active_region_summaryNOAA/USAF Solar Active Region Summary List
rhessi_hxr_flareRHESSI Hard X-ray Flare List
soho_pm_ip_shockSOHO/CELIAS/MTOF/PM Interplanetary Shock List
soho_eit_wave_transientSOHO/EIT Wave Transient List
soho_lasco_cmeSOHO/LASCO CME Event List
halo_cme_flare_magnetic_stormSOHO/LASCO Halo CME with assoc SGD H-alpha Flare and WDC Mag Storm List
solar_wind_eventSolar wind events
stereo_hi_cmeSTEREO Heliospheric Imager CME Event List
stereo_hi_sw_transientSTEREO/HI Solar Wind Transient List
stereo_euvi_eventSTEREO/SECCHI/EUVI Event List
timed_see_flareTIMED-SEE Flare Catalog
tsrs_solar_radio_eventTrieste Solar Radio System (TSRS) Solar Radio Event List
wind_typeii_soho_cmeType II Radio Burst (WIND) and Associated CME (SOHO) List
ulysses_hxr_flareUlysses Catalog of Solar Hard X-Ray Flares
ulysses_hxr_flare_farsideUlysses Catalog of Solar Hard X-Ray Flares on the Far-side of the Sun
ulysses_grb_xray_flareUlysses/GRB X-ray Flare List
ulysses_swoops_icmeUlysses/SWOOPS Interplanetary CME List
wind_ace_sirWind and ACE List SIRs List
wind_stereo_ii_iv_radioburstWIND and STEREO Candidate Type II and IV Radio Burst List
wind_mfi_bs_crossing_timeWIND/MFI Bow Shock Cross Crossing Time List
wind_mfi_ip_shockWIND/MFI Interplanetary Shock List
wind_mfi_mag_cloudWIND/MFI Magnetic Cloud List
yohkoh_sxt_trace_listYOHKOH SXT TRACE flare list
yohkoh_hxr_flareYohkoh/HXT Hard X-ray Flare List

aad_gle

AAD Ground Level Enhancement List


Purpose:
List of ground level events detected by ground-based neutron monitors
Description
Ground level enhancements (GLEs) are sudden increases in the cosmic ray intensity recorded by ground based detectors. GLEs are invariably associated with large solar flares but the acceleration mechanism producing particles of up to tens of GeV is not understood. The increases in ground based measurements ranges from only a few percent of background in polar monitors (with little or no geomagnetic cutoff) to 45 times for the 23 February 1956 event. The rate of GLEs would appear to be about one per year but there may be a slight clumping around solar maximum. Most solar flares associated with GLEs are located on the western sector of the Sun where the Interplanetary Magnetic Field (IMF) is well connected to the Earth. The geometry of this field line is quite variable, as it depends on the strength of the solar wind that varies considerably. Because of its shape it is known as the ``garden hose'' field line. GLEs associated with flares located near to the footpoint of the garden hose field line usually arrive promptly and have very sharp onsets. Conversely, GLEs associated with flares far from the garden hose field line are usually delayed in their arrival at Earth and have more gradual increases to maximum intensity. It is very rare to observe GLEs associated with flares to the east of the central meridian or Sun-Earth line. Although a large solar flare is invariably associated with a GLE the flare itself may not be causally related to the production of the high energy protons that produce the GLE response at Earth. Solar energetic particle events are not rare and energetic protons are produced in common with CMEs and interplanetary shocks. These protons do not have sufficient energy to produce secondary particles that reach ground level but are clearly observed by spacecraft. Such CMEs and their associated shocks are most often produced without a solar flare. It is possible that there is a continuum to the acceleration process and that flares are a by-product of the most energetic events. Alternatively, there is a possibility that the flare itself produces a seed population of higher energy protons that are further accelerated to energies sufficient to produce a GLE. (Ref: http://www.atnf.csiro.au/pasa/18_1/duldig/paper/node6.html)
Caveats
Acknowledgement/References
http://neutronm.bartol.udel.edu/~pyle/GLE_List.txt
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
comment ()
Comments
(UCD: meta.note, UTYPE: helio:comment)

cactus_soho_cme

CACTus SOHO/LASCO CME List


Purpose:
This list contains parameters describing coronal mass ejections (CMEs) autonomously detected by CACTus in image sequences from SOHO/LASCO.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/ Some information (such as position angle) depends on the observatory location.
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: )
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: )
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: )
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: )
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc;stat.median, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: phys.veloc;stat.correlation, UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.soho_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

cactus_soho_flow

CACTus SOHO/LASCO Flow List


Purpose:
This list contains parameters describing solar wind flows autonomously detected by CACTus in image sequences from SOHO/LASCO.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: helio:observatory_name)
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: helio:cme.duration_lift_off_h)
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: , UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.soho_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

cactus_stereoa_cme

CACTus STEREO-A/COR CME List


Purpose:
This list contains parameters describing coronal mass ejections (CMEs) autonomously detected by CACTus in image sequences from STEREO-A/COR.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: helio:observatory_name)
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: helio:cme.duration_lift_off_h)
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: , UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.stereoa_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

cactus_stereoa_flow

CACTus STEREO-A/COR Flow List


Purpose:
This list contains parameters describing solar wind flows autonomously detected by CACTus in image sequences from STEREO-A/COR.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: helio:observatory_name)
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: helio:cme.duration_lift_off_h)
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: , UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.stereoa_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

cactus_stereob_cme

CACTus STEREO-B/COR CME List


Purpose:
This list contains parameters describing coronal mass ejections (CMEs) autonomously detected by CACTus in image sequences from STEREO-B/COR.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: helio:observatory_name)
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: helio:cme.duration_lift_off_h)
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: , UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.stereob_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

cactus_stereob_flow

CACTus STEREO-B/COR Flow List


Purpose:
This list contains parameters describing solar wind flows autonomously detected by CACTus in image sequences from STEREO-B/COR.
Description
The CACTus software package (Computer Aided CME Tracking) was developed by the Solar Influences Data Center (SIDC) of the Royal Obervatory of Belgium; the project was co-funded by ESA (16913/03/NL/LvH).
Caveats
The CME list is automatically generated by CACTus; there is no human intervention or supervision at this stage. Caution should be used when employing the data for statistical purposes. See URLs http://www.sidc.be/cactus/ and http://secchi.nrl.navy.mil/cactus/
Acknowledgement/References
When any CACTus data are used please cite one of the following publications: http://adsabs.harvard.edu/abs/2004A%26A...425.1097R http://adsabs.harvard.edu/abs/2009ApJ...691.1222R
http://www.sidc.be/cactus/
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sat_id ()
The identifier of the spacecraft to which the list applies. The format of the ID follows the naming convention from the HELIO Instrument Catalogue Service (ICS).
(UCD: meta.id;instr.obsty, UTYPE: helio:observatory_name)
r_hci AU (1.496E+11>m) HCI
The heliocentric distance of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
The heliocentric latitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
The heliocentric longitude of the observatory (satid) for which the information is provided.
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Onset time, earliest indication of liftoff
(UCD: time.start, UTYPE: helio:time_period.time_start)
duration hours (3600>s)
Duration of liftoff (hours)
(UCD: time.duration, UTYPE: helio:cme.duration_lift_off_h)
pa degrees (1>degrees)
Position angle (degrees, counterclockwise from North)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Angular width of the CME (degrees)
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1000>ms-1)
Median velocity (km s-1)
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
dv km s-1 (1000>ms-1)
Variation (1 sigma) of velocity over the width of the CME
(UCD: , UTYPE: helio:cme.velocity.dv)
v_min km s-1 (1000>ms-1)
Lowest velocity detected within the CME
(UCD: phys.veloc;stat.min, UTYPE: helio:cme.velocity.v_min)
v_max km s-1 (1000>ms-1)
Highest velocity detected within the CME maxv Highest velocity detected within the CME
(UCD: phys.veloc;stat.max, UTYPE: helio:cme.velocity.v_max)
flag_halo ()
II if da greater than 90, III if da greater than 180, IV if da greater than 270, indicating potential halo/partial halo/CME ????
(UCD: meta.code, UTYPE: helio:cme.halo)
cme_number Unitless (1.0>Unitless)
CME number [[corresponds to column 'CME' in the original file without leading zeros]]
(UCD: meta.number, UTYPE: helio:cme.cme_number.stereob_cme_number)
event_detail ()
Link to details and graphs of specified CME [yymm-CME0010]
(UCD: meta.ref.url, UTYPE: helio:cme.event_detail_url)

stereo_impactplastic_icme

Catalogue of Interplanetary Coronal Mass Ejections from STEREO IMPACT/PLASTIC


Purpose:
The catalogue of Interplanetary Coronal Mass Ejections (ICMEs) from the Level 3 Results of STEREO IMPACT/PLASTIC.
Description
The ICMEs are identified based by inspection of a combination signatures: an enhancement of total perpendicular pressure, a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a declining solar wind speed, and a low proton temperature [Jian et al., 2006, Sol. Phy., 239, 393]. At least three of the above features were required to identify an ICME. The edges of ICMEs were identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties.
Caveats
The event list is only for reference purpose. Some of the events are still ambiguous as they often occur near HCS and/or SIR. In addition, there is no related particle data for all the events. For ambiguous event, please consult Lan Jian (lanjian@ucla.edu) or other scientists working on ICMEs. When there is a shock at the edge, the time is selected to the closest minute.
Acknowledgement/References
http://www-ssc.igpp.ucla.edu/~jlan/STEREO/Level3/STEREO_Level3_ICME.pdf
Parameters:
HEC_id HEC id (1.0>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
id Unitless (1.0>Unitless)
Event identifier (reset at beginning of year).
(UCD: meta.id, UTYPE: )
flag ()
? indicates an ambiguous event * indicates a hybrid event (i.e. Combined with another solar wind structure)
(UCD: meta.code, UTYPE: )
spacecraft ()
STEREO spacecraft A or B.
(UCD: instr.obsty, UTYPE: helio:observatory.observatory_name)
time_start UT (1.0>UT)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_mag_obstacle_start UT (1.0>UT)
tart time of magnetic obstacle (~ flux rope).
(UCD: time.start;phys.magField, UTYPE: )
time_end UT (1.0>UT)
End time of the event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
pt_max pPa (1.0E-12>kgm-1.s-2)
The maximum total pressure (Pt, sum of magnetic and perpendicular plasma thermal pressures) perpendicular to the magnetic field.
(UCD: phys.pressure;stat.max, UTYPE: )
pt_max_sheath pPa (1.0E-12>kgm-1.s-2)
Maximum Pt including the sheath region.
(UCD: phys.pressure;stat.max, UTYPE: )
b_max nT (1.0E-9>Tesla)
Maximum magnetic field measured in the event.
(UCD: stat.max;phys.magField, UTYPE: )
b_max_sheath nT (1.0E-9>Tesla)
Maximum magnetic field including the sheath region.
(UCD: stat.max;phys.magField, UTYPE: )
v_max km.s-1 (1000>m.s-1)
Maximum velocity.
(UCD: phys.veloc;stat.max, UTYPE: )
v_max_sheath km.s-1 (1000>m.s-1)
Maximum velocity including the sheath region.
(UCD: phys.veloc;stat.max, UTYPE: )
delta_v km.s-1 (1000>m.s-1)
Temporal variation of solar wind speed over one event, negative value indicating solar wind is expanding. No value means the solar wind speed remains almost constant over the event.
(UCD: arith.rate;phys.veloc, UTYPE: )
group Unitless (1.0>Unitless)
In the hypothesis that all ICMEs have a central flux rope, these three groups of Pt profiles are due to different approach distances to the central flux rope. Group 1 includes events that appear to be traversed near the ICME center, showing an apparent enhanced central Pt Group 3 represents ICMEs passed far away from the center, displaying a rapid rise and then gradual decay in Pt; Group 2 includes events with intermediate signatures.
(UCD: meta.code.class, UTYPE: )
comment ()
Short description of event.
(UCD: meta.note, UTYPE: helio:comment)

stereoa_impactplastic_shock

catalogue of Interplanetary Shocks from STEREO-A IMPACT/PLASTIC


Purpose:
The catalogue of Interplanetary Shocks from the Level 3 Results of STEREO-A IMPACT/PLASTIC.
Description
The forward and reverse shocks are identified using 8-Hz magnetic field data. We rotated them into shock normal coordinates to examine the existence of associated shock waves and field changes consistent with the Rankine-Hugoniot relations. The shock normal angle, field change, and Mach number, are also given in this list. To confirm, the 1-min PLASTIC data have also been checked. At forward shocks, all of solar wind speed, proton number density, proton temperature, and magnetic field should increase simultaneously. At reverse shocks, solar wind speed increases, while proton number density, proton temperature, and magnetic field all decrease. However, not all shocks have clear signatures in plasma properties. These shocks are indicated in the comments.
Caveats
Acknowledgement/References
http://www-ssc.igpp.ucla.edu/~jlan/STEREO/Level3/STEREO_Level3_Shock.pdf
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
id Unitless (1>Unitless)
Event identifier.
(UCD: meta.id, UTYPE: )
time_start UT (1.0>UT)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
mag_ratio Unitless (1.0>Unitless)
Ratio of downstream magnetic field intensity to upstream magnetic field intensity.
(UCD: arith.ratio;phys.magField, UTYPE: )
norm_angle degrees (1.0>degrees)
Shock normal angle.
(UCD: , UTYPE: )
beta Unitless (1.0>Unitless)
The ratio of plasma thermal pressure to magnetic pressure upstream of the shock.
(UCD: phys.magField;phys.pressure;arith.ratio, UTYPE: )
mach_no Unitless (1.0>Unitless)
Magnetosonic Mach number.
(UCD: phys.veloc;arith.ratio, UTYPE: )
data_avail ()
Y or N indicates the availability of 32-Hz MAG data for this shock.
(UCD: meta.code, UTYPE: )
f_r_shock ()
Forward(F)/Reverse(R) Shock.
(UCD: meta.code, UTYPE: )
comment ()
Short description of event.
(UCD: meta.note, UTYPE: helio:comment)

stereob_impactplastic_shock

Catalogue of Interplanetary Shocks from STEREO-B IMPACT/PLASTIC


Purpose:
The catalogue of Interplanetary Shocks from the Level 3 Results of STEREO-A IMPACT/PLASTIC.
Description
The forward and reverse shocks are identified using 8-Hz magnetic field data. We rotated them into shock normal coordinates to examine the existence of associated shock waves and field changes consistent with the Rankine-Hugoniot relations. The shock normal angle, field change, and Mach number, are also given in this list. To confirm, the 1-min PLASTIC data have also been checked. At forward shocks, all of solar wind speed, proton number density, proton temperature, and magnetic field should increase simultaneously. At reverse shocks, solar wind speed increases, while proton number density, proton temperature, and magnetic field all decrease. However, not all shocks have clear signatures in plasma properties. These shocks are indicated in the comments.
Caveats
Acknowledgement/References
http://www-ssc.igpp.ucla.edu/~jlan/STEREO/Level3/STEREO_Level3_Shock.pdf
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
id Unitless (1>Unitless)
Event identifier,
(UCD: meta.id, UTYPE: )
time_start time_start UT (1.0>UT)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
mag_ratio Unitless (1.0>Unitless)
Ratio of downstream magnetic field intensity to upstream magnetic field intensity.
(UCD: arith.ratio;phys.magField, UTYPE: )
norm_angle degrees (1.0>degrees)
Shock normal angle.
(UCD: , UTYPE: )
beta Unitless (1.0>Unitless)
The ratio of plasma thermal pressure to magnetic pressure upstream of the shock, assumed as 1 when there is data gap (DG).
(UCD: phys.magField;phys.pressure;arith.ratio, UTYPE: )
mach_no Unitless (1.0>Unitless)
Magnetosonic Mach number.
(UCD: phys.veloc;arith.ratio, UTYPE: )
data_avail ()
Y or N indicates the availability of 32-Hz MAG data for this shock.
(UCD: meta.code, UTYPE: )
f_r_shock ()
Forward(F)/Reverse(R) Shock.
(UCD: meta.code, UTYPE: )
comment ()
Short description of event.
(UCD: meta.note, UTYPE: helio:comment)

stereoa_impactplastic_sir

Catalogue of Stream Interaction Regions (SIRs) from STEREO-A IMPACT/PLASTIC


Purpose:
The catalogue of Stream Interaction Regions (SIRs) from the Level 3 Results of STEREO-A IMPACT/PLASTIC.
Description
The SIRs include corotating interaction regions (CIRs) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycle. The SIRs are identified based on inspection of the following features: an increase of solar wind speed, a pile-up of total perpendicular pressure (Pt) with gradual decreases at both sides from the Pt peak to the edges of interaction region, velocity deflections, an increase of proton number density, an enhancement of proton temperature, an increase of the entropy defined as ln(Tp3/2/Np) [Siscoe and Intriligator, 1993; Crooker et al., 1996], a compression of the magnetic field. We require the presence of at least 5 signatures, and identify SIRs with careful consideration of the ambient solar wind. For detail, please refer to Jian et al., 2006, Sol. Phy., 239, 337.
Caveats
Acknowledgement/References
http://www-ssc.igpp.ucla.edu/~jlan/STEREO/Level3/STEREO_Level3_SIR.pdf
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
comp_id (1>Unitless)
Comparison pair between spacecraft A and B (before 2008 when they were relatively close together).
(UCD: meta.id.cross, UTYPE: )
id (1>Unitless)
Event identifier (reset at beginning of year).
(UCD: meta.id, UTYPE: )
flag ()
* indicates a hybrid event combined by a SIR and another solar wind structure (e.g. an ICME). ? Indicates an ambiguous event.
(UCD: meta.code, UTYPE: )
spacecraft ()
STEREO spacecraft - A.
(UCD: instr.obsty, UTYPE: helio:observatory.observatory_name)
time_start UT (1.0>Unitless)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of the event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
time_pt_max UT (1.0>UT)
The approximate stream interface time, because it is where the forces at the two sides of the interface are equal and in opposite directions.
(UCD: time.phase;phys.pressure;stat.max, UTYPE: )
pt_max pPa (1.0E-12>kgm-1.s-2)
The maximum total pressure (Pt, sum of magnetic and perpendicular plasma thermal pressures) perpendicular to the magnetic field.
(UCD: phys.pressure;stat.max, UTYPE: )
b_max nT (1.0E-9>Tesla)
Maximum magnetic field in the event.
(UCD: stat.max;phys.magField, UTYPE: )
np_max cm-3 (1.0E+6>m-3)
Maximum proton number density in the event.
(UCD: phys.density;stat.max, UTYPE: )
v_min km.s-1 (1000>m.s-1)
Minimum velocity.
(UCD: phys.veloc;stat.min, UTYPE: )
v_max km.s-1 (1000>m.s-1)
Maximum velocity.
(UCD: phys.veloc;stat.max, UTYPE: )

stereob_impactplastic_sir

Catalogue of Stream Interaction Regions (SIRs) from STEREO-B IMPACT/PLASTIC


Purpose:
The catalogue of Stream Interaction Regions (SIRs) from the Level 3 Results of STEREO-B IMPACT/PLASTIC.
Description
The SIRs include corotating interaction regions (CIRs) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycle. The SIRs are identified based on inspection of the following features: an increase of solar wind speed, a pile-up of total perpendicular pressure (Pt) with gradual decreases at both sides from the Pt peak to the edges of interaction region, velocity deflections, an increase of proton number density, an enhancement of proton temperature, an increase of the entropy defined as ln(Tp3/2/Np) [Siscoe and Intriligator, 1993; Crooker et al., 1996], a compression of the magnetic field. We require the presence of at least 5 signatures, and identify SIRs with careful consideration of the ambient solar wind. For detail, please refer to Jian et al., 2006, Sol. Phy., 239, 337.
Caveats
Acknowledgement/References
http://www-ssc.igpp.ucla.edu/~jlan/STEREO/Level3/STEREO_Level3_SIR.pdf
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
comp_id Unitless (1>Unitless)
Comparison pair between spacecraft A and B (before 2008 when they were relatively close together).
(UCD: meta.id.cross, UTYPE: )
id Unitless (1>Unitless)
Event identifier (reset at beginning of year).
(UCD: meta.id, UTYPE: )
flag ()
* indicates a hybrid event combined by a SIR and another solar wind structure (e.g. an ICME). ? Indicates an ambiguous event.
(UCD: meta.code, UTYPE: )
spacecraft ()
STEREO spacecraft - B.
(UCD: instr.obsty, UTYPE: helio:observatory.observatory_name)
time_start UT (1.0>UT)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of the event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
time_pt_max UT (1.0>UT)
The approximate stream interface time, because it is where the forces at the two sides of the interface are equal and in opposite directions.
(UCD: time.phase;phys.pressure;stat.max, UTYPE: )
pt_max pPa (1.0E-12>kgm-1.s-2)
The maximum total pressure (Pt, sum of magnetic and perpendicular plasma thermal pressures) perpendicular to the magnetic field.
(UCD: phys.pressure;stat.max, UTYPE: )
b_max nT (1.0E-9>Tesla)
Maximum magnetic field of the event.
(UCD: stat.max;phys.magField, UTYPE: )
np_max cm-3 (1.0E+6>m-3)
Maximum proton number density.
(UCD: phys.density;stat.max, UTYPE: )
v_min km.s-1 (1000>m.s-1)
Minimum velocity.
(UCD: phys.veloc;stat.min, UTYPE: )
v_max km.s-1 (1000>m.s-1)
Maximum velocity.
(UCD: phys.veloc;stat.max, UTYPE: )

cme_forbush_event

CME-related Forbush Decrease Event List


Purpose:
List of Forbush decreases related to CMEs (Contributed by E Eroshenko, Izmiran)
Description
The magnetic field configurations propagating through the Heliosphere as Interplanetary Coronal Mass Ejections (ICMEs) also reduce the galactic cosmic ray flux. The count rates before an event are subtracted, and the rates given as a percentage of the count rate as compared to the average values measured before the event. The depressions can attain values of 20%. They are called Forbush decreases after the cosmic ray physicist Scott Forbush. The depressions of cosmic ray flux are ascribed to the shield produced by the complex and turbulent magnetic field structure in and around the ICME and the shock wave it drives ahead of it.
Caveats
All data are for Cosmic Rays of 10GV rigidity.
Acknowledgement/References
http://www.nmdb.eu/?q=node/135
Parameters:
HEC_id HEC id (1>unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
flag_ssc ()
Flag indicating if the onset of the event corresponds ("sc") to a Storm Sudden Commencement, otherwise the flag is left blank.
(UCD: meta.code, UTYPE: helio:forbush_decrease.flag_ssc)
fe_magn ()
Magnitude of 10 GV Cosmic Ray variation (in fact, magnitude of the FE)
(UCD: , UTYPE: helio:forbush_decrease.fe_magnitude)
kpmax Unitless (1>Unitless)
Maximum of the Kp-index in the associated geomagnetic deisturbance
(UCD: , UTYPE: helio:forbush_decrease.kp_max)
dst_min nT (1.0E-9>T)
Minimum of the Dst-index in the associated geomagnetic disturbance
(UCD: , UTYPE: helio:magnetic_storm.disturbance_storm_time)
b_max nT (1.0E-9>T)
Maximum of the magnitude of the Interplanetary Magnetic Field in the associated solar wind disturbance
(UCD: stat.max;phys.magField, UTYPE: helio:forbush_decrease.b_max)
vsw_max km.s-1 (1000>m.s-1)
Maximum of the solar wind speed in the associated solar wind disturbance
(UCD: phys.veloc;stat.max, UTYPE: helio:fobush_decrease.v_solar_wind.v_max)
axy_max percent (1.0>percent)
Maximum of the equatorial component of anisotropy during the Forbush Decrease.
(UCD: , UTYPE: helio:forbush_decrease.axy_min)
az_r ()
Range of change for the north-south component of anisotropy during the Forbush Decrease
(UCD: , UTYPE: helio:forbush_decrease.az_r)
tmin hours (3600>s)
Time from onset to the Forbush Decrease minimum
(UCD: time.duration;stat.min, UTYPE: helio:forbush_decrease.duration_to_min)
dc_min s-1 (1.0>s-1)
Maximum decrement between hourly counts of 10 GV Cosmic Rays
(UCD: meta.number;stat.min, UTYPE: helio:forbush_decrease.dc_min)
tdmn hours (3600>s)
Time from the onset to the maximum decrement in the 10 GV Cosmic Rays
(UCD: time.duration, UTYPE: helio:forbush_decrease.duration_to_max_decrement)
aftob ()
Ratio of the variation in the 10 GV cosmic rays to the maximum of the IMF intensity in the associated solar wind disturbance (fe_magn/bimf_m)
(UCD: , UTYPE: helio:fobush_decrease.fe_to_b)
tilt degrees (1.0>degrees) ???
Heliospheric current sheet tilt for day of the event
(UCD: , UTYPE: helio:forbush_decrease.tilt)

cme_inner_heliosphere

CMEs in the Inner Heliosphere


Purpose:
Catalogue of Large CMEs with LASCO Images and IPS Images in the Inner Heliosphere.
Description
The radial evolution of 30 large CMEs (angular width >150 degrees, i.e., halo and partial halo CMEs) has been investigated between the Sun and the Earth using (i) the white-light images of the near-Sun region from the Large Angle Spectroscopic Coronagraph (LASCO) onboard the SOHO mission and (ii) the interplanetary scintillation (IPS) images of the inner heliosphere obtained from the Ooty Radio Telescope (ORT).
Caveats
Acknowledgement/References
Manoharan, P.K,: 2006, Solar Phys, 235, 345
Parameters:
HEC_id Unitless (1>Unitless)
Event Identification number (HEC internal number).
(UCD: , UTYPE: )
cme_number ()
CME number.
(UCD: , UTYPE: )
time_start UT (1.0>UT)
The time that the CME was detected by SOHO LASCO.
(UCD: , UTYPE: )
v_cme km.s-1 (3.0E+3>m.s-1)
The initial speed of the CME derived from the 'height-time' plot from the LASCO images.
(UCD: , UTYPE: )
cme_type ()
"H" indicates a halo event and "PH" indicates a partial halo event.
(UCD: , UTYPE: )
xray_class x-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of associated flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: , UTYPE: )
optical_class ()
Average optical importance of associated flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field). "flm" indicates a filament eruption.
(UCD: , UTYPE: )
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of associated flare.
(UCD: , UTYPE: )
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of associated flare.
(UCD: , UTYPE: )
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of associated flare.
(UCD: , UTYPE: )
time_ips_1au UT (1.0>UT)
The time of arrival of the interplanetary shock at 1AU.
(UCD: , UTYPE: )
time_cme_1au UT (1.0>UT)
The time of arrival of the interplanetary CME (i.e. ejecta and/or magnetic cloud).
(UCD: , UTYPE: )
v_icme km.s-1 (3.0E+3>m.s-1)
The ICME speed at 1AU.
(UCD: , UTYPE: )
time_transit_1au h (3.6E+3>s)
The observed CME transit time from the Sun to 1AU.
(UCD: , UTYPE: )
alpha Unitless (1.0>Unitless)
The speed-distance slope from interplanetary scintillation measurements.
(UCD: , UTYPE: )
v_1au_predict km.s-1 (3.0E+3>m.s-1)
The predicted velocity of the ICME at 1 AU from the LASCO and interplanetary scintillation measurements.
(UCD: , UTYPE: )
time_transit_1au_predict h (3.6E+3>s)
The predicted CME transit time from the Sun to 1AU from the LASCO and interplanetary scintillation measurements.
(UCD: , UTYPE: )
flag_cme_interaction h (3.6E+3>s)
"Y" indicates that the CME interacts with other CMEs.
(UCD: , UTYPE: )

goes_proton_event

GOES Proton Event List


Purpose:
Geo-effective solar energetic proton (SEP) events (NOAA)
Description
Proton fluxes are integral 5-minute averages for energies >10 MeV, given in Particle Flux Units (pfu), measured by GOES spacecraft at Geosynchronous orbit: 1 pfu = 1 p cm-2 sr-1 s-1. The start of a proton event is identified based on the first of 3 consecutive data points with fluxes greater than or equal to 10 pfu. The end of an event is the last time the flux was greater than or equal to 10 pfu. It should be recognised that this definition allows multiple proton flares and/or interplanetary shock proton increases to occur within one SWO proton event. Additional data may be necessary to more completely resolve any individual proton event. Flare associations are given, although data about individual Coronal Mass Ejections (CMEs), available from SOHO since 1996 only, are necessary to fully characterize each event. CME information for earlier events from the SOLWIND and SMM coronagraphs will be added in the future.
Caveats
Different detectors, onboard different GOES spacecraft, have taken the data since 1976. These proton data were processed using various algorithms. To date, no attempt has been made to cross-normalize the resulting proton fluxes.
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time - the first of 3 consecutive data points with fluxes greater than or equal to 10 pfu.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Peak time
(UCD: time.phase, UTYPE: helio:time.time_peak)
proton_flux pfu (100>m-2sr-1s-1)
Proton fluxes are integral 5-minute averages for energies > 10 MeV, given in Particle Flux Units (pfu), measured by GOES spacecraft at Geosynchronous orbit: 1 pfu = cm-2 sr-1 s-1.
(UCD: prot.flux, UTYPE: helio:proton_event.proton_flux)
cme_parameters SOHO CME # (1>Unitless)
ID of a SOHO/LASCO identified CME associated with this event (available since 1996 only).
(UCD: , UTYPE: helio:comment)
time_peak_flare UT (1.0>UT)
The time of the peak in the associated X-ray flare.
(UCD: time.phase, UTYPE: helio:time.time_peak)
nar NAR # (1>Unitless)
The number for the closest NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Latitude of the associated active region
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Longitude of the associated active region
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
optical_class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)

goes_sxr_flare

GOES Soft X-ray Flare List


Purpose:
List of X-ray flares based on observations by the GOES spacecraft
Description
List generated by NOAA-SWPC based on observations in 0.1-0.8 nm from the XRS instrument on the GOES spacecraft. There are usually two GOES spacecraft operational resulting in virtually complete coverage since the 1970s. Recent segments of the catalogue can be found through the NOAA site; archive segments held by the NGDC.
Caveats
Acknowledgement/References
ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SOLAR_FLARES/FLARES_XRAY
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of flare
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Peak time of flare
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time of flare
(UCD: time.end, UTYPE: helio:time_period.time_end)
nar NAR # (1>Unitless)
NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of event
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Stonyhurst longitude of active region
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region
(UCD: pos, UTYPE: helio:location.long_carr)
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
optical_class Optical class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)

goes_flare_sep_event

GOES Strong Flares and associated SEP Events


Purpose:
List of X-class flares in the western solar hemisphere and the related findings of SEP from the GOES Space Environment Monitor_s Energetic Particle Sensor.
Description
The event list was created to invetigate why flares accompanied by intense soft X-ray bursts may not produce SEPs detected by observations with the GOES spacecraft. It consists of all X-class X-ray bursts between 1996 and 2006 from the western solar hemisphere and is taken from Appendix A of the paper by Klein et al, Solar Physics (2011) 269:309-333.
Caveats
Acknowledgement/References
Klein et al, Solar Physics (2011) 269:309-333.
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of the peak of the event.
(UCD: time.phase, UTYPE: time.time_peak)
time_end UT (1.0>UT)
End time of event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
loc_source ()
G indicates the location inferred from the Halpha observations as given in the GOES X-ray list. S indicates it is from the Solar Geophysical Data (SGD) Comprehensive Reports.
(UCD: meta.code;pos, UTYPE: )
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of x-ray flare.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of x-ray flare.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of x-ray flare.
(UCD: , UTYPE: location.long_carr)
optical_class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: flare.magnitude.optical_class)
xray_class x-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: flare.magnitude.xray_class)
time_start_rise_sep UT (1.0>UT)
Time at which the proton intensity starts to rise.
(UCD: time.epoch, UTYPE: )
upper_limit Unitless (1>Unitless)
Y if the peak integral proton intensity is an upper limit - N if not.
(UCD: meta.code;stat.max, UTYPE: )
intensity_sep_peak pfu (10000>m-2sr-1s-1)
The peak integral proton intensity at energies above 10 MeV.
(UCD: stat.max;prot.flux, UTYPE: )
intensity_sep_exp pfu (10000>m-2sr-1s-1)
For upper limits for the intensity, the expected value of the integral intensity above 10 MeV as defined, based on the soft X-ray properties, by Equation (6) of Garcia (2004), Space Weather, 2, S02002.
(UCD: prot.flux, UTYPE: proton_event.proton_flux)
comment ()
If the event is in the SEP list complied by NOAA, it is indicated by NOAA and a time. A capital C indicates a 'confined' event associated with CME-less X-class bursts. There are five categories of events: (a) 21 SEP events that were catalogued by NOAA based on GOES observations. (b) 10 SEP events detected by GOES that were not catalogued because their peak intensity did not exceed the threshold of 10 pfu. (c) 8 prominent GOES SEP events that were not catalogued because the intensity at event onset was already above the threshold of 10 pfu due to a previous event. 5 further weak SEP events were identified on top of previous excess intensities labelled _(c')_. (d) GOES/EPS showed no excess signal above background after 15 X-class flares, and six further cases where no new rise was detected on top of a high intensity from a previous event (labelled _(d')_). (u) In four cases the GOES SEP detection was uncertain because of the high background from energetic storm particles (ESP) or because of possible confusion of SEP signatures with a previous event.
(UCD: meta.note, UTYPE: helio:comment)

istp_sw_event

ISTP Solar Wind Candidate Event List


Purpose:
ISTP solar wind catalogue candidate events.
Description
The events in the list correspond to one or more of several features observed by the IMP-8, WIND and ACE spacecraft. These features include: BzN - Interplanetary magnetic B-field North (GSM coordinate system) BzS - Interplanetary magnetic B-field South (GSM coordinate system) EyC - Change of the "y" component of the Interplanetary Electric Field HSS - High Speed Stream IMC - Interplanetary Magnetic Cloud IR - Interaction Region IS - Interplanetary Fast Shock LSS - Low Speed Stream PC - Pressure Change SBC - Sector Boundaries Crossing, also heliospheric current sheet crossing MISC - Miscellaneous Events
Caveats
Acknowledgement/References
http://www-spof.gsfc.nasa.gov/scripts/sw-cat/Catalog_events.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
category ()
Category of event - one or more of the following features separated by a /. BzN - Interplanetary magnetic B-field North (GSM coordinate system) A B-field North event is defined as an extended period of magnetic field oriented northward. Presently the catalog includes only those BzN events that extend for periods longer than 4 hours, within which only brief southward excurtions may occur. BzS - Interplanetary magnetic B-field South (GSM coordinate system) A B-field South event is defined as an extended period of magnetic field oriented southward. Presently the catalog includes under this entry only those BzS events that extend for periods longer than 4 hours, within which only brief Northward violations may occur. EyC - Change of the "y" component of the Interplanetary Electric Field Included are the observed events characterized by a sudden sign change and large amplitude variation in Ey (Ey=Bz*Vx) (the dawn to dusk component of the interplanetary electric field). HSS - High Speed Stream An HSS is defined as a SW flow moving outward from the Sun with a high speed (usually a bulk velocity Vb>500 km s-1), accompanied by low density and high temperature protons. Presently the catalog includes only those HSS events that extended for periods longer than a day. IMC - Interplanetary Magnetic Cloud An Interplanetary Magnetic Cloud is defined as (1) a smooth variation of the magnetic field direction, through a large angle; (2) strong magnetic fields; and (3) low ion temperature and low proton beta; all occurrring on a time scale of about 1 day or so. IR - Interaction Region Region of approximately half a day or longer showing unusually high magnetic and plasma pressures. IS - Interplanetary Fast Shock An IS is defined in term of simultaneous changes in the bulk velocity (Vb) of the SW ions, their thermal velocity (Vth), and density (n) as well as the magnitude of the magnetic field (|B|), (and sometimes its direction), so that the Rankine-Hugoniot equations are expected to be satisfied for the event. Fast forward shocks, those most commonly seen in the interplanetary medium at 1 AU, are identified by positive changes in all of these quantities in time. Strong IS accompanied by a Southward oriented B-field have been associated with the observance of strong geomagnetic storms. The catalog contains only "candidates" for the IS category, based in the observations of the sudden change in the B-field and plasma quantities that within the resolution of the available KPs can be interpreted as being consistent with an interplanetary shock. LSS - Low Speed Stream Only those periods of LSS when the Vb<330 km s-1 are included. An occassional feature of a LSS is the presence of multiple SBCs (see def. Below), and PC disruptions. PC - Pressure Change These are PCs other than IS. PC is defined as the sudden or gradual change (i.e. Over a short period of time; usually less than an hour) in the type of the SW pressure (+ or -), i.e., between kinetic and the magnetic field pressures. There may or may not be pressure equilibrium accross this region during the change. SBC - Sector Boundaries Crossing, also heliospheric current sheet crossing A SBC is identified by an usually rapid change in field direction by 180+/-60 Degs. Such that the field goes from one relatively stable direction (over several days) to another after the change(s). Sometimes this transition occurs after a large (and odd) number of such crossings, for many hours. Commonly there is a brief dip in field intensity (magnetic hole) at a crossing. MISC - Miscellaneous Events Events/Information deemed relevant to Solar, SW, or magnetospheric studies but failing to fit the other categories are added to the catalog under the MISC category.
(UCD: meta.code.class, UTYPE: helio:solar_wind.category)
spacecraft ()
Spacecraft - can be one or more of 8 (for IMP-8), W (for WIND) and ACE.
(UCD: instr.obsty, UTYPE: helio:observatory.observatory_name)
comment ()
Comments
(UCD: meta.note, UTYPE: helio:comment)

kso_halpha_flare

Kanzelhoehe Solar Observatory (KSO) H-alpha Flare List


Purpose:
Flares observed in H-alpha by the Kanzelhoehe Observatory.
Description
The list contains the following information for each flare: observed beginning of the flare observed maximum of the flare observed end of the flare heliographic position of the flare Type: area (importance) [S, 1, 2, 3] and brightness [F, N, B] of the flare
Caveats
Acknowledgement/References
http://www.kso.ac.at/beobachtungen/sonne_daten/flares_en.php
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Observed beginning of flare.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_start_m ()
Time modifier: E means Earlier U means Uncertain D means Later
(UCD: meta.code, UTYPE: helio:flare.time_start_modifier)
time_peak UT (1.0>UT)
Observed maximum of flare.
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_peak_m ()
Time modifier: E means Earlier U means Uncertain D means Later
(UCD: meta.code, UTYPE: helio:flare.time_peak_modifier)
time_end UT (1.0>UT)
Observed end of the flare.
(UCD: time.end, UTYPE: helio:time_period.time_end)
time_end_m ()
Time modifier: E means Earlier U means Uncertain D means Later
(UCD: meta.code, UTYPE: helio:flare.time_end_modifier)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of flare
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of flare
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region.
(UCD: pos, UTYPE: helio:location.long_carr)
optical_class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)

goes_flare_no_sep_radio_cme

List of Radio and CME associations for GOES flares without SEP


Purpose:
List of all western X-class flares that were not accompanied by SEP detected by GOES/EPS.
Description
The times have been re-evaluated using GOES 3s data. The start time is given as the time, rounded to the nearest minute, where the derivative of the flux starts to be persistently positive in either the 0.05 _ 0.4 nm channel or the 0.1 _ 0.8 nm channel, depending on which is earliest. The coincidence of this onset time with a local minimum in the flux profile has been verified by visual inspection. Properties of the microwave emission were taken from Solar Geophysical Data or, whenever data were available on line, derived from an analysis of the whole Sun patrol observations of the RSTN network (observing frequencies: 15.4, 8.8, 4.995, 2.695, 1.415, 0.610, 0.410 and 0.245 GHz) and the Nobeyama Radio Polarimeters with observing frequencies 35, 17, 9.4, 3.75, 2.0, 1.0 GHz (Nakajima et al., 1985). In some events, data from the University of Bern patrol observations (courtesy A. Magun) were also used. The information on decametric-hectometric (DH) type III bursts was inferred from the Wind/WAVES observations at the highest observed frequency (13.8 MHz), through the evaluation of the instrument background. The indicated duration is the time interval during which the observed flux density was three standard deviations above the background level. In the 13 August 2004 event no outstanding type III burst was observed by the highfrequency detector of WAVES, but a delayed one was clearly visible at lower frequencies (below 1MHz). Its onset time is given, although the association with the flare is questionable because of the long delay and the low starting frequency. It is taken from Appendix B of the paper by Klein et al, Solar Physics (2011) 269:309-333. For the information on the existence and timing of an associated CME, the catalogues of LASCO CMEs (http://cdaw.gsfc.nasa.gov/CME_list/) and of EIT dimmings or waves (http://solar.nro.nao.ac.jp/norp/) wwere used. The numerical values are the times when the backwards extrapolated time-height trajectory of the CME front is at 0 and 1 solar radius, respectively. In cases without LASCO observations or when the estimated CME start was different from the flare time and the detection or potential detection of a dimming listed in the NEMO catalogue. The 9 July 1996 CME was only detected when it was well above the limb, and the backwards extrapolation is uncertain. Values in the table are quoted from Dryer et al. (1998) and Pick et al. (1998). A similar uncertainty occurs with the CME on 3 July 2002. The flare on 27 November 1999 occurred between several other flare/CME events in the same quadrant. The corona as seen by SoHO/LASCO is highly variable and makes new CMEs hard to identify.
Caveats
Acknowledgement/References
Klein et al, Solar Physics (2011) 269:309-333.
Parameters:
HEC_id Unitless (1>Unitless)
Event Identification number (HEC internal number).
(UCD: , UTYPE: )
time_start UT (1.0>UT)
Start time of flare.
(UCD: , UTYPE: )
time_peak UT (1.0>UT)
Time of flare maximum.
(UCD: , UTYPE: )
cutoff_hf GHz (1.0E+9>s-1)
High-frequency cut-off. * indicates that it is based on microwave patrol reports compiled in Solar Geophysical Data.
(UCD: , UTYPE: )
time_spec_peak UT (1.0>UT)
Time of the spectral maximum.
(UCD: , UTYPE: )
frequ_spec_peak GHz (1.0E+9>s-1)
Frequency of the spectral maximum.
(UCD: , UTYPE: )
flux_spec_peak sfu (1.0E-22>Wm-2Hz-1)
Flux density at the spectral maximum.
(UCD: , UTYPE: )
cutoff_lf_hi GHz (1.0E+9>s-1)
High end of the low frequency cut-off range where the event is visible.
(UCD: , UTYPE: )
cutoff_lf_lo GHz (1.0E+9>s-1)
Low end of the low frequency cut-off range where the event is invisible.
(UCD: , UTYPE: )
alpha_lf Unitless (1.0>Unitless)
Spectral index at low frequencies.
(UCD: , UTYPE: )
deci_metre_waves ()
A rough characterisation of the radio emission at decimetre-to-metre wavelengths (frequency range 600 _ 30 MHz), as compiled from Solar Geophysical Data and from observatory web sites.
(UCD: , UTYPE: )
time_start_dh_typeIII UT (1.0>UT)
Start time of DH type III burst.
(UCD: , UTYPE: )
time_end_dh_typeIII UT (1.0>UT)
End of DH type III burst.
(UCD: , UTYPE: )
n_bursts Unitless (1>Unitless)
Number of individual bursts.
(UCD: , UTYPE: )
comment_dh_typeIII ()
Comment on DH type III burst.
(UCD: meta.note, UTYPE: helio:comment)
flag_dimming ()
Y when CME times are determined by dimming, otherwise it is N.
(UCD: , UTYPE: )
time_start_cme UT (1.0>UT)
Time at which the backwards extrapolated time-height trajectory of the CME front is at 0.
(UCD: , UTYPE: )
time_cme_solar_radius UT (1.0>UT)
Time at which the backwards extrapolated time-height trajectory of the CME front is at 1 solar radius.
(UCD: , UTYPE: )
cme_speed km.s-1 (1.0E+3>ms-1)
Projected speed of CME.
(UCD: , UTYPE: )
pa_width degrees (1.0>degrees)
Angular width of the CME.
(UCD: , UTYPE: )
comment_cme ()
Comments on the CME.
(UCD: meta.note, UTYPE: helio:comment)

mars_earth_icme

Mars Earth ICME List


Purpose:
List of ICME events detected at Mars and the Earth
Description
The events in this list were taken from Table 1 in the paper Falkenberg et al, Space Weather 9, S00E12 (2011). They represent in situ data taken from the MGS satellite, the OMNI database and the GOES satellites. Shock times are read from data plots of MGS data and OMNI data. The SOHO/LASCO catalogue was used to try to identify the CME source of the observed shocks. The max values are the maximum value measured within 12 hours of shock arrival.
Caveats
Negative heliocentric longitudinal distances indicate that Mars was trailing Earth. Only those events which could be identified in the SOHO/LASCO catalogue have been included in the list.
Acknowledgement/References
Falkenberg et al, Space Weather 9, S0012 (2011)
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
event_id HEC id (1>Unitless)
ICME event identifier in paper.
(UCD: meta.id, UTYPE: )
time_start_mars UT (1.0>UT)
Start of shock event at Mars.
(UCD: time.start, UTYPE: time.time_start)
p_dyn_mars nPa (1.0E-9>kgm-1,s-2)
The maximum solar wind (particle) dynamic pressure at Mars (MGS).
(UCD: phys.pressure;stat.max, UTYPE: )
counts_max_mars s-1 (1>s-1)
The maximum background count rate in the Electron Re flectometer on MGS.
(UCD: phys.energy;stat.max;meta.number, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
time_start_earth UT (1.0>UT)
Start of shock event at the Earth.
(UCD: time.start;pos.earth, UTYPE: time.time_start)
p_dyn_earth nPa (1.0E-9>kgm-1,s-2)
The maximum dynamic pressure at Earth (OMNI).
(UCD: phys.pressure;stat.max;pos.earth, UTYPE: )
v_max_earth km.s-1 (1000>m.s-1)
The maximum speed of CME at Earth (OMNI).
(UCD: phys.veloc;stat.max;pos.earth, UTYPE: )
density_max_earth cm-3 (1.0E+6>m-3)
The maximum density of CME at Earth (OMNI).
(UCD: phys.density;stat.max;pos.earth, UTYPE: )
counts_max_goes s-1 (1.0>s-1)
The maximum GOES signal (>30MeV).
(UCD: phys.energy;stat.max, UTYPE: )
long_hci_sepn degrees (1.0>degrees)
The heliocentric longitude distance between Earth and Mars.
(UCD: pos.bodyrc.long;pos.heliocentric;pos.distance, UTYPE: )

icme_earth_cycle23

Near-Earth Interplanetary Coronal Mass Ejections During Solar Cycle 23


Purpose:
Catalogue of near-Earth Interplanetary Coronal Mass Ejections (ICMEs) over the complete cycle 23 (1996-2009).
Description
The catalogue summarises the basic properties and geomagnetic effects. In particular, solar wind composition and charge state observations are now considered when identifying the ICMEs. In general, these additional data confirm the earlier identifications based predominantly on other solar wind plasma and magnetic field parameters. However, the boundaries of ICME-like plasma based on charge state/composition data may deviate significantly from those based on conventional plasma/magnetic field parameters. Furthermore, the much studied _magnetic clouds_, with flux-rope-like magnetic field configurations, may form just a substructure of the total ICME interval.
Caveats
Acknowledgement/References
Richardson, I.G., Cane, H.V.: 2010, Solar Phys 264, 189
Parameters:
HEC_id Unitless (1>Unitless)
Event Identification number (HEC internal number).
(UCD: , UTYPE: )
time_start UT (1.0>UT)
The start time of the ICME-related _disturbance_. For a fast ICME, this is given by the arrival of the ICME-driven shock. In this case, the time given is typically that of the geomagnetic storm sudden commencement (SC) that frequently accompanies a shock reaching the Earth_s magnetosphere since this provides a spacecraft-independent arrival time that is also appropriate for comparison with phenomena at the Earth.
(UCD: , UTYPE: )
time_start_icme UT (1.0>UT)
The start time of the ICME. The ICME start time is inferred primarily from plasma and magnetic field data and given to the nearest hour.
(UCD: , UTYPE: )
time_end_icme UT (1.0>UT)
The end time of the ICME. The ICME end time is inferred primarily from plasma and magnetic field data and given to the nearest hour.
(UCD: , UTYPE: )
flag_a_w ()
If a sudden commencement (SC) is reported this flag is not set. If an SC is not reported, the time of shock passage at ACE (indicated by (A)) is given. If there are no data at ACE, or a shock is not reported at that spacecraft, the shock time at WIND (W) is listed if a shock is reported. If no shock is reported for a slower ICME, a wave-like feature or developing shock may be evident in the plasma and field data. The time of such a feature is given in the table to the nearest hour.
(UCD: , UTYPE: )
time_offset_start_sig h (3600>s)
Estimated offset of the start of the compositional/charge state signatures in the vicinity of the ICME relative to the _ICME_ start time.
(UCD: , UTYPE: )
flag_toff_start_sig ()
_ns_ indicates that there is no compositional/charge state signature while _nc_ indicates that there is no change or there is no clear compositional/charge state change. An absence of data is indicated by _nd _. Close agreement between the ICME and composition/ charge state boundaries (to within an hour or so, limited by the resolution of the SWICS data) is indicated by a _zero hour_ offset. Different compositional/charge state changes may not coincide exactly though frequently there is a consensus. Typically the O7/O6 ratio is used as a reference.
(UCD: , UTYPE: )
time_offset_end_sig h (3600>s)
Estimated offset of the end of the compositional/charge state signatures in the vicinity of the ICME relative to the _ICME_ end time.
(UCD: , UTYPE: )
flag_toff_end_sig ()
_ns_ indicates that there is no compositional/charge state signature while _nc_ indicates that there is no change or there is no clear compositional/charge state change. An absence of data is indicated by _nd _. Close agreement between the ICME and composition/ charge state boundaries (to within an hour or so, limited by the resolution of the SWICS data) is indicated by a _zero hour_ offset. Different compositional/charge state changes may not coincide exactly though frequently there is a consensus. Typically the O7/O6 ratio is used as a reference.
(UCD: , UTYPE: )
time_offset_start_mc h (3.6E+3>s)
Time offset (in hours) of the magnetic leading boundary relative to the ICME boundary based primarily on the WIND magnetic cloud list. Additional events identified by Huttunen et al. (2005) in 1996 _ 2003 are also included.
(UCD: , UTYPE: )
flag_toff_start_mc ()
"nd" indicates an absence of data.
(UCD: , UTYPE: )
time_offset_end_mc h (3.6E+3>s)
Time offset (in hours) of the magnetic trailing boundary relative to the ICME boundary based primarily on the WIND magnetic cloud list. Additional events identified by Huttunen et al. (2005) in 1996 _ 2003 are also included.
(UCD: , UTYPE: )
flag_toff_end_mc ()
"nd" indicates an absence of data. "2" indicates that two magnetic clouds are identified in the interval of interest. The offsets are then estimated from the leading edge of the first magnetic cloud and the trailing edge of the second.
(UCD: , UTYPE: )
bidir_flow_e ()
Indicates whether or not bidirectional suprathermal electrons were observed within the ICME (Y/N = yes/no), based on an assessment of the SWEPAM electron pitchangle plots from the ACE Science Center. For events before the launch of ACE, and events where SWEPAM observations are dominated by solar energetic particles, the 260 eV electron pitch-angle plots from the WIND 3DP instrument (http://sprg.ssl.berkeley.edu/wind3dp/) were examined. In a few cases, indicated by _SEP_, it was not possible to assess the presence of BDEs in either data set because of the presence of solar energetic particles. Overall, 67% of the ICMEs (205/308), where an assessment can be made, data show evidence of BDEs.
(UCD: , UTYPE: )
bidir_flow_ion ()
Indicates the presence of bidirectional energetic ion flows (BIFs) observed by the IMP 8 GME (for the ICME commencing on 31 October 2003, the BIFs are reported by Malandraki et al. (2005)). Here, _. nd _ indicates that either there are no data for a given ICME, the available data cover a limited region of the ICME such that it is not possible to assess whether any bidirectional flows were present, particle counts are insufficient to be able to assess the particle flows, or IMP 8 was inside the bow shock. _Y_ or _N_ indicate that there is, or is no, evidence (in the available data, which may not extend throughout the ICME interval) of bidirectional flows. Overall, energetic ion flows can be examined for 114 ICMEs, of which 66 (58%) show evidence of BIFs.
(UCD: , UTYPE: )
qual_time_est ()
indicates the overall _quality_ of the ICME boundary time estimates, where _1_ is the most reliable.
(UCD: , UTYPE: )
flag_weak_event ()
_W_ indicates a marginal event with weak ICME signatures.
(UCD: , UTYPE: )
v_incr_sw km.s-1 (3.0E+3>m.s-1)
The increase in solar wind speed at the upstream disturbance (to the nearest 10 km s_1) estimated from 1-hour averaged data.
(UCD: , UTYPE: )
flag_upstream_shock ()
An _S_ indicates that a shock reported in the ACE or Kasper shock lists contributed to the speed increase (which may be larger than the actual speed increase at the shock if for example, the solar wind speed increased further following the shock). Of the 322 ICMEs, 163 (51%) have identified upstream shocks. Note that in a few cases (e.g., 4 May 1998), there is a large increase in solar wind speed but no shock is reported. Typically, the speed transition is too gradual to be associated with a true shock.
(UCD: , UTYPE: )
v_mean_sw km.s-1 (3.0E+3>m.s-1)
The average ICME speed based on the plasma/field ICME intervals.
(UCD: , UTYPE: )
v_max_sw km.s-1 (3.0E+3>m.s-1)
The maximum post-shock solar wind speed (i.e., between the shock/disturbance and plasma/field ICME trailing edge),
(UCD: , UTYPE: )
b_mean nT (1.0E-9>T)
The average magnetic field strength within the plasma/field ICME, to the nearest 1 nT.
(UCD: , UTYPE: )
flag_mag_cloud ()
A _2_ indicates that the ICME includes a magnetic cloud reported on the WIND magnetic cloud list. In a few cases, an indicated magnetic cloud is not reported on these lists, but the magnetic field characteristics of the ICME are assessed to be consistent with those for a magnetic cloud (e.g., enhanced intensity >10 nT, smooth rotation through a large angle, low proton temperatures, Klein and Burlaga, 1982). A _1_ indicates that there is evidence of a rotation in the magnetic fielddirection, but overall, the magnetic field characteristics do not meet those of a magnetic cloud. Events with no magnetic cloud-like magnetic field features are indicated by _0_.
(UCD: , UTYPE: )
flag_mc_list ()
'H' indicates a magnetic cloud reported by Huttunen et al. (2005).
(UCD: , UTYPE: )
dst_min nT (1.0E-9>T)
The minimum geomagnetic Dst.
(UCD: , UTYPE: )
flag_dst ()
_P_ indicates that the value is provisional, and _Q_ that the value is obtained from the _Real-time (Quicklook)_ Dst index provided by the World Data Center for Geomagnetism, Kyoto University (http://swdcwww.kugi.kyoto-u.ac.jp/). Otherwise, final values are given. The period considered for each event extends from the disturbance to the trailing edge of the ICME signatures or slightly beyond if a storm driven by the trailing regions of an ICME reaches peak intensity just after ICME passage. A null value indicates that strong geomagnetic activity is already in progress and there is no further intensification associated with the ICME.
(UCD: , UTYPE: )
v_1au km.s-1 (3.0E+3>m.s-1)
The shock transit speed to 1 AU if the probably associated solar event can be identified. If so details are given in the following fields.
(UCD: , UTYPE: )
time_lasco UT (1.0>UT)
The event time generally corresponding to the first observation of the related CME by the LASCO coronagraphs on the SOHO spacecraft.
(UCD: , UTYPE: )
flag_halo ()
"H" denotes that this is reported as a halo CME in the online CME catalogue (http://cdaw.gsfc.nasa.gov/CME_list/). "dg" indicates a gap in LASCO observations that encompasses the likely time of the associated solar event. SOHO EIT movies and other data (e.g., H_ flares) are used to help infer the solar source regions of the CMEs. "F" indicates an associated solar flare if there are no LASCO observations. In some cases, there are multiple CMEs, but the time of the most likely association is given.These are indicated by "?". "(S)" indicates observations of Earthward-directed CMEs made by the SECCHI coronagraphs on the STEREO spacecraft (http://secchi.nrl.navy.mil/).
(UCD: , UTYPE: )

ngdc_aastar_storm

NGDC AA* Major Magnetic Storm List


Purpose:
List of major magnetic storms according to the AA* criteria (NGDC)
Description
Daily regular magnetic field variation arise from current systems caused by regular solar radiation changes. Other irregular current systems produce magnetic field changes caused by the interaction of the solar wind with the magnetosphere, by the magnetosphere itself, by the interactions between the magnetosphere and ionosphere, and by the ionosphere itself. Magnetic activity indices were designed to describe variation in the geomagnetic field caused by these irregular current systems The aa-index is a simple global geomagnetic activity index. It is derived from the K indices from two approximately antipodal observatories and has units of 1 nT. The K-index is quasi-logarithmic local index of the 3-hourly range in magnetic activity relative to an assumed quiet-day curve for a single geomagnetic observatory site. First introduced by J. Bartels in 1938, it consists of a single-digit 0 thru 9 for each 3-hour interval of the universal time day (UT). This list has been produced at WDC-A for STP, a now-routine procedure is to take the 3-hourly aa indices when they are received and compute an 8-point running average. When this mean exceeds 60, a "major magnetic" storm is considered to be in progress. It is arbitrarily considered to continue in progress until such time as the value drops below a threshold of 60. Then the maximum mean value attained is designated AA*.
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of onset of magnetic storm.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of maximum AA*.
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time of the magnetic storm.
(UCD: time.end, UTYPE: helio:time_period.time_end)
duration hours (3600.0>s)
Duation of event in hours
(UCD: time.duration, UTYPE: )
aastar_max AA* (1>(AA*))
Maximum AA* during the event.
(UCD: , UTYPE: helio:magnetic_storm.aastar_max)
aastar_ave AA* (1>(AA*))
Average AA* value over the event.
(UCD: , UTYPE: helio:magnetic_storm.aastar_average)
aastar_sum AA* (1>(AA*))
AA* sum.
(UCD: , UTYPE: helio:magnetic_storm.aastar_sum)

ngdc_apstar_storm

NGDC Ap* Major Magnetic Storm List


Purpose:
List of major magnetic storms according to the Ap* criteria (NGDC)
Description
Daily regular magnetic field variation arise from current systems caused by regular solar radiation changes. Other irregular current systems produce magnetic field changes caused by the interaction of the solar wind with the magnetosphere, by the magnetosphere itself, by the interactions between the magnetosphere and ionosphere, and by the ionosphere itself. Magnetic activity indices were designed to describe variation in the geomagnetic field caused by these irregular current systems. The 3-hourly ap (equivalent range) index is derived from the Kp index. The planetary 3-hour-range index Kp is the mean standardized K-index from 13 geomagnetic observatories between 44 degrees and 60 degrees northern or southern geomagnetic latitude - for the conversion from Kp to ap, see http://www.ngdc.noaa.gov/stp/geomag/kp_ap.html. The Ap* index is defined as the earliest occurring maximum 24-hour value obtained by computing an 8-point running average of successive 3-hour ap indices during a geomagnetic storm event and is uniquely associated with the storm event. At WDC-A for STP, a now-routine procedure is to take the 3-hourly ap indices when they are received and compute the 8-point running average. When this mean exceeds 40, a "major magnetic storm" is considered to be in progress. It is arbitrarily considered to continue in progress until such time as the value drops below a threshold of 40. Then the maximum mean value attained is designated Ap*. When the most disturbed 24-hours begin at the start of the UT-day, the values of Ap and Ap* are identical.
Caveats
Acknowledgement/References
http://www.ngdc.noaa.gov/stp/GEOMAG/apstar.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of onset of magnetic storm.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of maximum Ap*.
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time of magnetic storm.
(UCD: time.end, UTYPE: helio:time_period.time_end)
duration hours (3600>s)
Duation of magnetic storm in hours.
(UCD: time.duration, UTYPE: helio:magnetic_storm.duration)
apstar_max Ap* (1>(Ap*))
Maximum Ap* during the event.
(UCD: , UTYPE: helio:magnetic_storm.apstar_max)
apstar_ave Ap* (1>(Ap*))
Average Ap* value over the event.
(UCD: , UTYPE: helio:magnetic_storm.apstar_average)
apstar_sum Ap* (1>(Ap*))
Ap* sum.
(UCD: , UTYPE: helio:magnetic_storm.apstar_sum)

ngdc_halpha_flare

NGDC H-alpha Flare List


Purpose:
List of H-alpha flares assembled from ground-based observatories (NGDC)
Description
Flares are characterized by a rise time of the order of minutes and a decay of the order of tens of minutes. The total energy released in a typical flare is about 1027 J; the magnetic field is extraordinarily intense, reaching values of 10-2 to 1 Tesla. This list is constructed by NGDC from the basic reports sent monthly from the ground-based observatories. The National Geophysical Data Center (NGDC) holds archives for about 80 stations, covering the period 1938 to the present. Currently 5 stations send their data to NGDC Boulder on a routine monthly basis. Optical flares in H-alpha are usually accompanied by radio and X-ray bursts, and occasionally by high-energy particle emissions.
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Earliest Universal Time of flare onset reported within a group.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Earliest Universal Time within group that flare reached maximum brightness
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
Average of flare end times
(UCD: time.end, UTYPE: helio:time_period.time_end)
nar NAR # (1>Unitless)
NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Average heliographic latitude marking the mean center of mass of the flaring region at its time of maximum brightness.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Average heliographic longitude of active region marking the mean center of mass of the flaring region at its time of maximum brightness.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of the flaring region.
(UCD: pos, UTYPE: helio:location.long_carr)
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
optical_class Optical class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)

ngdc_ssc

NGDC Storm Sudden Commencement List


Purpose:
List of the onset of geo-magnetic storms (NGDC)
Description
SEC defines geomagnetic storms based on the running Boulder A-index. If the index is greater than or equal to 30, a storm is in progress. The running A-index is calculated using the K indices in a running 24-hour window, rather than using fixed days. Storms are minor, major, or severe as defined below. minor: A+B between 30 and 49 major: A+B between 50 and 99 severe: A+B 100 or greater
Caveats
However, the level of storm conditions can vary throughout a day. Regardless of the running A-index, it is permissible to say that periods at minor, major, or severe storm levels occurred, based on the observed K index. The following table identifies K indices with storm levels. minor storm conditions: K=5 major storm conditions: K=6 severe storm conditions: K=7 or greater
Acknowledgement/References
ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SUDDEN_COMMENCEMENTS/storm2
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Begin time for sudden storm commencement.
(UCD: time.start, UTYPE: helio:time_period.time_start)
nstn_a Unitless (1>Unitless)
Number of stations reporting an A event. Letter A -- denotes very remarkable event observed.
(UCD: meta.number, UTYPE: helio:magnetic_storm.number_stations_a)
nstn_b Unitless (1>Unitless)
Number of stations reporting a B event. Letter B -- denotes fair, ordinary, but unmistakable event observed.
(UCD: meta.number, UTYPE: helio:magnetic_storm.number_stations_b)
nstn_c Unitless (1>Unitless)
Number of stations reporting a C event. Letter C -- denotes very poor, doubtful event observed.
(UCD: meta.number, UTYPE: helio:magnetic_storm.number_stations_c)
nsi Unitless (1>Unitless)
Number of stations reporting an "si" event. Letters "si" -- sudden impulse event (sudden magnetic change which could not be classified as ssc (sudden storm commencement), bs, etc.)
(UCD: meta.number, UTYPE: helio:magnetic_storm.number_stations_si)

noaa_energetic_event

NOAA Solar Energetic Event List


Purpose:
List of energetic solar events, plus radio observations assembled from the daily Solar and Geophysical Activity Summary (SGAS) reports (NOAA)
Description
A list of significant solar events including start, maximum, and end times, region number and location, X-ray and optical classification of flares, significant radio emission at 245 MHz, 2695 MHz (11 cm), and sweep frequencies, and significant short wave fades. All available data for an event are if one or more of the following thresholds are reached: Class-M or greater X-ray flare, Optical flare of importance > 2B, Radio burst of > 100 sfu at 245 MHz, Radio burst > 100% above background at 2695 MHz, Type II or IV sweep frequency burst, Shortwave fade of importance 2 or greater.
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Peak time
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time
(UCD: time.end, UTYPE: helio:time_period.time_end)
nar NAR # (1>Unitless)
NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of the active region
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Stonyhurst longitude of active region
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region
(UCD: pos, UTYPE: helio:location.long_carr)
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
optical_class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)
radio_245mhz ()

(UCD: em.radio.200-400MHz, UTYPE: helio:radio.radio_245mhz)
radio_10cm ()

(UCD: em.radio.1500-3000MHz, UTYPE: helio:radio.radio_10cm)
radio_sweep_ii ()
Type II sweep frequency
(UCD: em.radio, UTYPE: helio:radio.radio_sweep_ii)
radio_sweep_iv ()
Type IV sweep frequency
(UCD: em.radio, UTYPE: helio:radio.radio_sweep_iv)
swf ()
Shortwave fade
(UCD: meta.code, UTYPE: helio:radio.shortwave_fade)

noaa_active_region_summary

NOAA/USAF Solar Active Region Summary List


Purpose:
Parameters describing active regions: lat, long, size... (NOAA/USAF)
Description
The Solar Region Summary (SRS), compiled by SWPC, is a daily report of the active solar regions observed during the preceding day. The SRS contains a detailed description of the active regions currently visible on the solar disk. See sample and description below. The characteristics for each active region are compiled from up to six observatories that report to the SWPC in near-real time. The sunspot counts are typically higher than those reported in non-real time by the Sunspot Index Data Center (SIDC), Brussels, Belgium, and the American Association of Variable Star Observers.
Caveats
Acknowledgement/References
ftp://ftp.swpc.noaa.gov/pub/forecasts/SRS
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
nar NAR # (1>Unitless)
NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees)

(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees)
Heliographic Longitude.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region
(UCD: pos, UTYPE: helio:location.long_carr)
area ()
Total corrected area of the group in millionths of the solar hemisphere.
(UCD: phys.area, UTYPE: helio:ar.area)
zurich_class (1>Unitless)
Modified Zurich classification of the group.
(UCD: meta.code.class, UTYPE: helio:ar.zurich_class)
p_value ()
?
(UCD: stat.value, UTYPE: helio:ar.p_value)
c_value ()
?
(UCD: stat.value, UTYPE: helio:ar.c_value)
dlong_hg degrees (1.0>degrees)
?
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:ar.dlong_hg)
n_spots Unitless (1.0>Unitless)
Number of sunspots.
(UCD: meta.number, UTYPE: helio:ar.number_spots)
mag_class Unitless (1>Unitless)
Magnitude class
(UCD: meta.code.class;phot.mag, UTYPE: helio:ar.magnetic_class)

rhessi_hxr_flare

RHESSI Hard X-ray Flare List


Purpose:
List of hard X-ray flares seen by RHESSI.
Description
The RHESSI flare list is created during quicklook processing (and is often re-processed). The flare list is obtained by comparing the observing summary count rate in the 6 to 12 keV energy band to a threshold. The count rate threshold is determined from the background level; which is obtained using a 60 second running average. For an interval to be considered as a flare candidate, the count rate must be greater than 3*sigma above the background level. Variations in the count rate due to changes in attenuator state or decimation state are taken into account by use of the "corrected" count rate method, which empirically determines the corrections. A flare candidate is flagged as a possible solar flare if the ratio of the count rate in the front detectors to total count rate is 3 sigma above its own background level (also determined using a 60 second running average). An exception is made if there is an SAA crossing or data gap; for those cases the front - total ratio must be greater than 60% in the interval for that interval to be considered to be a possible flare. Even with the front - total ratio test, particle precipitation events can be confused with flares. The candidate is only confirmed as a solar flare if a valid position is found in the 6 to 12 keV energy band.
Caveats
Acknowledgement/References
http://hesperia.gsfc.nasa.gov/ssw/hessi/dbase/
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time determined from when the flux rate in the 6-12 keV band exceeds 3*sigma above the background level calcualted on a 60s running average.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
The time of the peak flux for the flare in the energy range greater than 6 keV
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time determined from when the flux rate in the 6-12 keV band drops below 3*sigma of the background level calcualted on a 60s running average.
(UCD: time.end, UTYPE: helio:time_period.time_end)
nar NAR # (1>Unitless)
The number for the closest NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
x_cart arcsec (2.7778E-4>degrees)
Position in arcsecs from centre of the sun.
(UCD: pos.cartesian.x;pos.bodyrc;pos.heliocentric/heliographic ?, UTYPE: helio:location.x_cart)
y_cart arcsec (2.7778E-4>degrees)
Position in arcsecs from centre of the sun.
(UCD: pos.cartesian.y;pos.bodyrc;pos.heliocentric/heliographic ?, UTYPE: helio:location.y_cart)
radial_arcsec arcsec (2.7778E-4>degrees)
Radial distance in arcsecs from the centre of the Sun.
(UCD: pos.heliographic/heliocentric?;pos.distance, UTYPE: helio:location.radial_arcsec)
duration s ()
Duration of the flare in seconds
(UCD: time.duration, UTYPE: helio:flare.duration)
count_sec_peak Unitless (1>Unitless)
Peak counts/second in energy range 12-25 keV, averaged over active collimators, including background.
(UCD: phot.count, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
total_count Unitless (1>Unitless)
Total counts in energy range 12-25 keV integrated over duration of flare summed over all subcollimators, including background.
(UCD: meta.number, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
energy_kev keV (1.602E-16>J)
The highest energy band in which the flare was observed.
(UCD: phys.energy, UTYPE: helio:flare.magnitude.hard_xray_quantifier.energy_keV)
flare_number Unitless (1>Unitless)
An ID number, ymmddnn, e.g., 2042101 is the first flare found for 21-Apr-2002. These numbers are not time ordered, e.g., flare 2042129 occurred before 2042104. Also all sorts of problems have been noted since 2010 has started, and the energy range has been changed, resulting in more than 100 flares in certain days. Flare_ids for 2010 and beyond start with a 2 digit year, and there can be 3 digits for the flare number in a given day e.g., 100601102.
(UCD: meta.id, UTYPE: helio:flare.rhessi_flare_number)

soho_pm_ip_shock

SOHO/CELIAS/MTOF/PM Interplanetary Shock List


Purpose:
An incomplete list of possible Interplanetary Shocks observed by the SOHO PM.
Description
The Shockspotter program attempts to identify possible interplanetary shocks using the near-real time data from the CELIAS/MTOF/PM sensor on the SOHO spacecraft. There are several reasons for developing automated procedures for identifying various interplanetary structures; for example the online capability of such techniques would be a useful addition to a space weather warning system, and could be used by spacecraft to make on-board decisions to change modes of operation. In addition, the objectivity of such an automated identification system is a benefit for unbiased statistical analyses. Rigorously, shocks cannot be identified using solely solar wind proton data; one needs electron and minor ion measurements in addition to magnetic field measurements (there is no magnetometer on SOHO). Nevertheless, a reasonable system of identification of at least the larger shocks is possible using only the PM data. This simplified Table lists the expected behavior of solar wind parameters across some common interplanetary structures: Vsw Np Vth B fast FWD shock increases increases increases increases fast REV shock increases decreases decreases decreases slow FWD shock increases increases increases decreases slow REV shock increases decreases decreases increases classical CME TD/CD steady decreases decreases increases classical high-speed increases decreases increases decreases stream
Caveats
Acknowledgement/References
http://umtof.umd.edu/pm/FIGS.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of shock.
(UCD: time.start, UTYPE: helio:time_period.time_start)
zone Unitless (1>Unitless)
Zone of shock, which indicates the likelihood of the event being a shock. There are 2 questions one must ask: 1) How many of the events found by Shockspotter are actually shocks? The "percentage shocks" entries given in the table below were derived by comparing the Shockspotter output for the 6-year period from Jan 21, 1996 to March 31, 2002 with the shock events listed on the "Figs" web page. The shock events listed on that page were originally subjectively identified by eye, and then checked to be at least consistent with the magnetic field behavior from either the ACE or WIND spacecraft. Since some of those identifications may be incorrect, the stated "percentage shocks" is only approximate. The Confidence Level is derived a bit more conservatively by decreasing the "# shocks" entries by 1 for each category. In general, a stronger shock will fall into a higher Zone than a weaker shock, and a shock detected during quiet pre-existing solar wind conditions wil fall into a higher zone than one detected during turbulent conditions. Type Zone # Events # shocks percentage shocks Confidence Level Forward 1 38 17 45% 42% Forward 2 28 20 71% 68% Forward 3 36 34 94% 92% Forward 4 67 67 100% 99% Reverse 1 13 6 46% 38% 2) How many shocks are missed by Shockspotter? This is a much more difficult question to answer. There are 105 forward or reverse shocks from 21 Jan 1996 to 21 Jan 2001 listed on the "Figs" page (as of this writing), of which 93 were found by Shockspotter. However, the shock list on the "Figs" page is far from complete; there are undoubtedly many weaker shocks that were not identified with this subjective procedure. For example, one of the Shockspotter tests requires a minimum speed jump of about 25 km s-1 (this minimum required jump speed is actually a function of density, see here for details). If one asks "How many relatively large shocks are missed by Shcoksptter?", then one can estimate that less than 10% of shocks of sufficient strength to reach Zone category 2 or higher are undetected by Shockspotter.
(UCD: meta.code.class, UTYPE: helio:solar_wind.ip_shock_zone)
comment ()
Comments.
(UCD: meta.note, UTYPE: helio:comment)

soho_eit_wave_transient

SOHO/EIT Wave Transient List


Purpose:
Waves seen in the EUV by SOHO/EIT.
Description
Abstract taken from 'A CATALOG OF CORONAL "EIT WAVE" TRANSIENTS' by B. J. Thompson and D. C. Myers, The Astrophysical Journal Supplement Series 183 (2009) 225. Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet Imaging Telescope (EIT) data have been visually searched for coronal "EIT wave" transients over the period beginning from 1997 March 24 and extending through 1998 June 24. The dates covered start at the beginning of regular high-cadence (more than 1 image every 20 minutes) observations, ending at the four-month interruption of SOHO observations in mid-1998. One hundred and seventy six events are included in this catalog. The observations range from "candidate" events, which were either weak or had insufficient data coverage, to events which were well defined and were clearly distinguishable in the data. Included in the catalog are times of the EIT images in which the events are observed, diagrams indicating the observed locations of the wave fronts and associated active regions, and the speeds of the wave fronts. The measured speeds of the wave fronts varied from less than 50 to over 700 km s^_1 with "typical" speeds of 200-400 km s^_1. URL for paper: http://iopscience.iop.org/0067-0049/183/2/225/apjs_183_2_225.text.html
Caveats
Acknowledgement/References
http://iopscience.iop.org/0067-0049/183/2/225/apjs300645t3.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of event (same as Image Time)
(UCD: time.start, UTYPE: helio:time_period.time_start)
previmg_time UT (1.0>UT)
Time of previous image.
(UCD: time.creation, UTYPE: helio:time.time)
img_time UT (1.0>UT)
Image Time.
(UCD: time.creation, UTYPE: helio:time.time)
quality ()
Quality Rating: Q0: Very low reliability; Q1: Low reliability; Q2: Low reliability; Q3: Intermediate reliability; Q4: High reliability; Q5: Nearly definite reliability;
(UCD: meta.code.class, UTYPE: helio:eit.quality)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic Latitude
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic Longitude. (A source longitude of 90 or _90 indicates that the apparent source of the wave was either at, above, or possibly behind the solar limb.)
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
v_ps km s-1 (1.0E+3>ms-1)
Speed of wave-front on the plane of the sky.
(UCD: phys.veloc, UTYPE: helio:eit.velocity.v_plane_of_sky)
v_proj km s-1 (1.0E+3>ms-1)
Speed of wave front assuming the wave travels in a great circle along the Sun's photosphere.
(UCD: phys.veloc, UTYPE: helio:eit.velocity.v_projected)
pa degrees (1.0>degrees)
Direction of Measurement on the photosphere expressed as a position angle (measured N through E) in relation to the Sun-Earth line..
(UCD: pos.posAng, UTYPE: helio:location.pa)
comment ()
Comments.
(UCD: meta.note, UTYPE: helio:comment)

soho_lasco_cme

SOHO/LASCO CME Event List


Purpose:
Edited list of CMEs detected by the LASCO instrument on SOHO (NASA/GSFC)
Description
This CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. This catalog contains all CMEs manually identified since 1996 from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) mission. LASCO has three telescopes C1, C2, and C3. However, only C2 and C3 data are used for uniformity because C1 was disabled in June 1998.
Caveats
The list is necessarily incomplete because of the nature of identification. In the absence of a perfect automatic CME detector program, the manual identification is still the best way to identify CMEs. Link to the list of data gaps during the month is also provided. Data gaps of duration 3 h or more are listed. The data-gap list must be consulted before deciding the existence or nonexistence of CMEs. If there is a data gap, it is difficult to say there was a CME or not during the data gap.
Acknowledgement/References
http://cdaw.gsfc.nasa.gov/publications/gopal2008.catalog.pdf
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time - the time of first appearance in the LASCO/C2 field of view.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time
(UCD: time.end, UTYPE: helio:time_period.time_end)
pa degrees (1.0>degrees)
Central position angle for the CME
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_measure degrees (1.0>degrees)
The position angle at which the height-time measurements are made (MPA for measurement position angle).
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_measure)
pa_width degrees (1.0>degrees)
Position angle width of the CME
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v km s-1 (1.0E+3>ms-1)
the linear speed obtained by fitting a straight line to the height-time measurements made at the fastest section of CMEs
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
v_init km s-1 (1.0E+3>ms-1)
quadratic speed obtained by fitting a parabola and evaluating the speed at the initial time of the event
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v_init)
v_final km s-1 (1.0E+3>ms-1)
quadratic speed obtained by fitting a parabola and evaluating the speed at the time of final height measurement
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v_final)
v_20r km s-1 (1.0E+3>ms-1)
quadratic speed obtained by fitting a parabola and evaluating the speed at 20 solar radii
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v_20r)
accel m s-2 (1.0>ms-2)
Acceleration is obtained from the quadratic fit to the height-time measurements
(UCD: phys.acceleration, UTYPE: helio:cme.acceleration)

halo_cme_flare_magnetic_storm

SOHO/LASCO Halo CME with assoc SGD H-alpha Flare and WDC Mag Storm List


Purpose:
List of Halo CMEs and associated flares and geomagnetic storms.
Description
Three sets of information are listed: (i) halo coronal mass ejections (CMEs), (ii) Associated flares and (iii) Associated geomagnetic storms. The halo CME list is obtained from the SOHO/LASCO CME catalog (http://cdaw.gsfc.nasa.gov/CME_list). The solar source location for each halo is obtained as the location of the associated H-alpha flare location if available from the online Solar Geophysical Data. Otherwise, the flare is identified by playing superposed LASCO and EIT movies along with GOES plots and deriving the heliographic coordinates of the associated flare from SOHO/EIT images. The minimum value of the Disturbance Storm Time (Dst) index is obtained from the World Data Center in Kyoto (http://swdcdb.kugi.kyoto-u.ac.jp/dstdir/). A 4-day long time window was chosen starting at CME onset+1 day and ending at CME onset + 5 days. The minimum value of Dst index in this time window after is halo CME is assigned to the halo CME.
Caveats
Acknowledgement/References
http://cdaw.gsfc.nasa.gov/CME_list)
Parameters:
HEC_id HEC id (1>Unitless)

(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of the CME
(UCD: time.start, UTYPE: helio:time_period.time_start)
cme_speed km s-1 (1000>ms-1)
Speed of the CME
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
pa_measure degrees (1.0>degrees)
Measurement Position Angle (MPA) at which CME height-time measurement was made.
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_measure)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Latitude solar source location of the CME heliographic coordinates given for frontside halos.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1>degrees) Stonyhurst Heliographic
Latitude solar source location of the CME heliographic coordinates given for frontside halos.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of the CME
(UCD: pos, UTYPE: helio:location.long_carr)
pos_flag ()
If the CME source location is on the Earthward side of the solar disk then this entry will be blank and the postion will be given in the the latitude and longitude fields. Otherwise flag will take one of the following values: "Backside": The source is behind the Sun "B?": The source is most likely backside. There may be some disk activity, but not associated with the CME "Blimb": The source is behind the limb, with subscripts E, W, NE, NW, SE, SW indicating the limb position from which the CME moves out. There is usually a dimming signature above the limb from which we infer that the eruption took place behind the limb.
(UCD: meta.code, UTYPE: helio:cme.position_description)
time_flare UT (1.0>UT)
Time of the associated GOES X-ray flare
(UCD: time.epoch, UTYPE: helio:flare.time_peak)
xray_class X-ray Class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
time_storm UT (1.0>UT)
Time of the associated geomagnetic storm correspodning to the time of minimum Dst index.
(UCD: time.epoch, UTYPE: helio:magnetic_storm.time_peak)
dst nT (1.0E-9>T)
Minimum Dst value.
(UCD: , UTYPE: helio:magnetic_storm.disturbance_storm_time)

solar_wind_event

Solar wind events


Purpose:
List of solar wind events observed upstream of the Earth
Description
The ISTP Science Planning and Operations Facility (SPOF), in collaboration with ISTP investigators, is developing this catalog of preliminary/selected solar wind events and features. The catalog also contains listings of times when WIND and IMP-8 were in the solar wind. Coverage begins on September 8, 1992, the start of ISTP science data collection. With the launch of ACE in 1997, and its permanent coverage of solar wind conditions in near real time we incorporate to our selection interesting time periods also observed with the instruments SWEPAM and MAG in ACE. The solar wind features are classified into several categories (e.g., interplanetary shock wave, extended period of strong negative Bz, etc.). An extended event has separate start and end times listed for it, whereas a sharp discontinuous event (such as a shock ramp) has the same time listed for both start and end times (clearly, for follow-up studies researchers will need to examine data before and after the listed time).
Caveats
The catalog contains information on selected features of the solar wind at 1 AU whose signatures derive from plasma and magnetic field measurements from the IMP-8 and WIND spacecraft in the form of Key Parameters (KPs -- preliminary summary data at ~1 min time resolution produced quickly for survey purposes); as such, the catalog should not be used a definitive source in formal scientific work. Researchers using the catalog should reference its contents with statements such as: The event from "Feb 26, 1995" has been identified as a candidate "Sector Boundary Crossing" worthy of further study. The primary intent for the catalog is to serve as a reference for identifying candidate periods for further study, such as may be the focus of coordinated data analysis efforts during ISTP and/or IACG Science Campaigns. The list should not be considered as comprehensive.
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
sw_list ()
The specific event category that the feature has been associated with
(UCD: meta.code.class, UTYPE: )
time_start UT (1.0>UT)
Start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time
(UCD: time.end, UTYPE: helio:time_period.time_end)
flag_bzn ()
Strong northward Bz for extended period Interplanetary magnetic B-field North (GSM coordinate system) A B-field North event is defined as an extended period of magnetic field oriented northward
(UCD: meta.code, UTYPE: )
flag_bzs ()
Strong southward Bz for extended period Interplanetary magnetic B-field South (GSM coordinate system) A B-field South event is defined as an extended period of magnetic field oriented southward
(UCD: meta.code, UTYPE: )
eyc ()
Change in Ey=VxBz Change of the "y" component of the Interplanetary Electric Field Included are the observed events characterized by a sudden sign change and large amplitude variation in Ey (Ey=Bz*Vx) (the dawn to dusk component of the interplanetary electric field.
(UCD: meta.code, UTYPE: )
flag_hss ()
Very high speed stream for extended period High Speed Stream An HSS is defined as a SW flow moving outward from the Sun with a high speed (usually a bulk velocity Vb>500 km s-1), accompanied by low density and high temperature protons.
(UCD: meta.code, UTYPE: )
flag_imc ()
Interplanetary magnetic cloud An Interplanetary Magnetic Cloud is defined as (1) a smooth variation of the magnetic field direction, through a large angle; (2) strong magnetic fields; and (3) low ion temperature and low proton Beta; all occurrring on a time scale of about 1 day or so.
(UCD: meta.code, UTYPE: )
flag_ir ()
Interaction Region Region of approximately half a day or longer showing unusually high magnetic and plasma pressures
(UCD: meta.code, UTYPE: )
flag_is ()
Interplanetary shock Interplanetary Fast Shock An IS is defined in term of simultaneous changes in the bulk velocity (Vb) of the SW ions, their thermal velocity (Vth), and density (n) as well as the magnitude of the magnetic field (|B|), (and sometimes its direction), so that the Rankine-Hugoniot equations are expected to be satisfied for the event. Fast forward shocks, those most commonly seen in the interplanetary medium at 1 AU, are identified by positive changes in all of these quantities in time. Strong IS accompanied by a Southward oriented B-field have been associated with the observance of strong geomagnetic storms.
(UCD: meta.code, UTYPE: )
flag_lss ()
Very low speed stream for extended period
(UCD: meta.code, UTYPE: )
flag_pc ()
Pressure change These are PCs other than IS. PC is defined as the sudden or gradual change (i.e. over a short period of time; usually less than an hour) in the type of the SW pressure (+ or -), i.e., between kinetic and the magnetic field pressures. There may or may not be pressure equilibrium across this region during the change.
(UCD: meta.code, UTYPE: )
flag_sbc ()
Interplanetary sector boundary crossings (usually in a set) Sector Boundaries Crossing, also heliospheric current sheet crossing A SBC is identified by an usually rapid change in field direction by 180+/-60 degs. such that the field goes from one relatively stable direction (over several days) to another after the change(s).
(UCD: meta.code, UTYPE: )
flag_misc ()
Miscellaneous, which may include a very broad range of features Events/Information deemed relevant to solar, SW, or magnetospheric studies but failing to fit the other categories are added to the catalog under the MISC category.
(UCD: meta.code, UTYPE: )
flag_w ()
Feature seen on the WIND spacecraft
(UCD: meta.code, UTYPE: )
flag_i8 ()
Feature seen on the IMP-8 spacecraft
(UCD: meta.code, UTYPE: )
flag_ace ()
Feature seen on the ACE spacecraft
(UCD: meta.code, UTYPE: )
comment ()
Comment about the observed solar wind feature.
(UCD: meta.note, UTYPE: helio:comment)

stereo_hi_cme

STEREO Heliospheric Imager CME Event List


Purpose:
List of CME events identified using the STEREO heliospheric imager instrument (RALspace)
Description
This list was compiled by Richard Harrison (RALspace) through careful inspection of the images obtained from the STEREO HI cameras. As such it is a more detailed list of CMEs, linking each to the appropriate transients seen in the "stereo_hi_sw_transient" where possible. The list contains information about direction and extent of each CME in terms of solar position angle. Since the process of visual identification of CMEs is time-consuming, this list is currently only complete for CMEs occurring to the end of 2008.
Caveats
The "time_start" and "time_end" correspond to the times that the CME was seen to enter and leave (or fade) from the STEREO HI field of view. Since STEREO A (Ahead) and B (Behind) are in heliocentric orbits their view angle with respect to the Sun-Earth line varies with time from the start of the mission.
Acknowledgement/References
http://www.sstd.rl.ac.uk/stereo/Events%20Page.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time - approximate time that CME enters HI field of view.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time - approximate time CME front leaves HI field of view.
(UCD: time.end, UTYPE: helio:time_period.time_end)
instrument ICS id (1>unitless)
This is the ID of the instrument on STEREO that was used to identify the event.
(UCD: instr, UTYPE: helio:instrument)
data_gap ()
Indication of a data gap during the event
(UCD: meta.code, UTYPE: helio:cme.data_gap)
cme_type ()
Classification of the CME type
(UCD: meta.code.class, UTYPE: helio:cme.cme_type)
brightness ()
Classification of the CME brightness
(UCD: , UTYPE: helio:cme.brightness)
pa degrees (1.0>degrees)
Central position angle for the observed CME
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width degrees (1.0>degrees)
Position angle width of the CME
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
time_onset UT (1.0>UT)
Estimated onset time for the event
(UCD: time.phase, UTYPE: helio:cme.time_onset)
not_in_list ()
Flag to indicate if the event is in the HI solar event list
(UCD: , UTYPE: )
v km s-1 (1.0E+3>ms-1)
Fitted CME speed.
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Fitted Stonyhurst longitude of the event
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_err degrees (1.0>degrees) Stonyhurst Heliographic
Error in the fitted longitude measurement
(UCD: pos.bodyrc.long;pos.heliographic;meta.code.error, UTYPE: helio:location.long_err)
time_1au UT (1.0>UT)
Time at which the CME was expected to reach 1 AU based on fitted time elongation profile
(UCD: time.phase, UTYPE: helio:time.time_1au)
comment ()
Description of the CME feature
(UCD: meta.note, UTYPE: helio:comment)

stereo_hi_sw_transient

STEREO/HI Solar Wind Transient List


Purpose:
List of STEREO/HI solar wind transient events
Description
This list contains speeds and directions calculated from time-height 'j-plots' along the ecliptic for all solar wind transients that are seen to propagate into the outer H12 cameras field of view. As this list is derived semi-automatically it contains speeds and directions for both coronal mass ejections (CMEs) and co-rotating interaction (CIRs) and does not distinguish between them.
Caveats
Acknowledgement/References
http://www.sstd.rl.ac.uk/Stereo/HIEventList.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
date ()
Date that event appears in H12 cameras field of view expressed as YYYY-MM-DD.
(UCD: time.phase, UTYPE: helio:time.time)
instrument ()
Instrument: STEREO_A__HI or STEREO_B__HI.
(UCD: instr, UTYPE: helio:instrument)
v km s-1 (1.0E+3>ms-1)
Velocity of the event.
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v)
v_err km s-1 (1.0E+3>ms-1)
Uncertainty in velocity.
(UCD: phys.veloc;stat.error, UTYPE: helio:solar_wind.velocity_proton_error.v_proton)
long_hg degrees (1.0>degrees)
Longitude from S-E line.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_err degrees (1.0>degrees)
Uncertainty in longitude from S-E line.
(UCD: pos.bodyrc.long;pos.heliographic;meta.code.error, UTYPE: helio:location.long_err)
time_start UT (1.0>UT)
Estimated launch time of event (assuming instant acceleration).
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_1au UT (1.0>UT)
Predicted time of arrival at 1 AU.
(UCD: time.phase, UTYPE: helio:time.time_1au)

stereo_euvi_event

STEREO/SECCHI/EUVI Event List


Purpose:
STEREO/EUVI Event Catalog (>C1 GOES class or >12 keV RHESSI)
Description
This is a catalogue of flare/CME events observed with EUVI when the spacecraft separation angle is small to moderate when classical stereoscopy is feasible. The list contains also the peak fluxes in soft X rays and hard X rays.
Caveats
Acknowledgement/References
http://secchi.lmsal.com/EUVI/euvi_catalog.txt
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
id_num (1>Unitless)
STEREO/EUVI event Catalogue Number.
(UCD: meta.id.cross, UTYPE: helio:externale_reference_id)
time_start UT (1.0>UT)
Start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time
(UCD: time.end, UTYPE: helio:time_period.time_end)
lat_hg degrees (1.0>degrees)
Heliographic Latitude.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees)
Heliographic Longitude.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region
(UCD: pos, UTYPE: helio:location.long_carr)
cadence s (1.0>s)
Instrument cadence.
(UCD: , UTYPE: helio:instr.cadence_s)
spacecraft s (1.0>s)
Spacecraft ID
(UCD: instr.obsty, UTYPE: helio:observatory.observatory_name)
xray_class Unitless ()
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
rhessi_peak_range keV (1.602E-16>J)
Peak RHESSI energy range in which event is observed.
(UCD: phys.energy;stat.max;inst.bandwidth, UTYPE: helio:flare.magnitude.hard_xray_quantifier.energy_range_keV)
rhessi_peak_count Unitless (1.0>Unitless)
Counts in peak RHESSI energy range.
(UCD: phys.energy;stat.max;meta.number, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
comment ()
Comments using the following EUVI Classification: A=Ahead only without Behind data B=Behind only without Ahead data I=Impulsive time profile (peak in coincidence with SXR) P=Postflare loop or arcade (delayed emission after SXR peak) D=Dimming (EUV flux decreases after SXR peak) E=Eruptive filament O=Occulted for A (if flare position is east) or B (if west) T=Test images (or poor image quality) W=Waves and oscillations
(UCD: meta.note, UTYPE: helio:comment)
cme_event_source ()
CME reported by one or both of the following: L=LASCO/SOHO S=SECCHI/Cor-1,Cor-2
(UCD: instr, UTYPE: helio:observatory_name)

timed_see_flare

TIMED-SEE Flare Catalog


Purpose:
Catalog of Flare Events observed by the TIMED-SEE experiment.
Description
This page is a catalog of flare events observed by the TIMED Solar EUV Experiment (SEE). Each row contains NOAA SEC flare information from the daily edited event reports for periods when TIMED-SEE was observing the sun anywhere between the start and stop times of these events. Events have been filtered to exclude periods when no appreciable increases were detected by SEE.
Caveats
Catalog last updated on Wed Sep 26 16:47:09 2007.
Acknowledgement/References
http://lasp.colorado.edu/see/see_flare_catalog.html
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of the event provided by the NOAA-SEC daily event report.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of event peak provided by the NOAA-SEC daily event report.
(UCD: time.phase, UTYPE: time.time_peak)
time_end UT (1.0>UT)
Time at the end of the event provided by the NOAA-SEC daily event report.
(UCD: time.end, UTYPE: helio:time_period.time_end)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of x-ray flare defined by SXI or H-alpha when no SXI location is reported.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of x-ray flare defined by SXI or H-alpha when no SXI location is reported.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of x-ray flare.
(UCD: , UTYPE: location.long_carr)
xray_class x-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: flare.magnitude.xray_class)
nar NAR # (1>Unitless)
NOAA active region index.
(UCD: meta.id.cross, UTYPE: flare.nar)
nevent Unitless (1>Unitless)
NOAA Event number.
(UCD: meta.number, UTYPE: )
see_xps_index Unitless (1>Unitless)
SEE-XPS Index - TIMED-SEE XPS (0.1-7 nm) Flare Index (1=no flare, >1=flare).
(UCD: meta.code;em.X-ray, UTYPE: )
see_egs_index Unitless (1>Unitless)
TIMED-SEE EGS Flare Index (1=no flare, >1=flare).
(UCD: meta.code;em.UV, UTYPE: )
obs_time_offset s (1>s)
Center of the TIMED-SEE observation time relative to the flare peak expressed in seconds. SEE observations are approximately 180 seconds. Positive numbers indicate seconds after the peak, negative numbers indicate seconds prior to the peak.
(UCD: time.duration, UTYPE: )
url_ftp_file ()
Link pointing to the SEE level 3A (observation avg) data file that contains the measurement closest to the peak.
(UCD: meta.ref.url, UTYPE: )

tsrs_solar_radio_event

Trieste Solar Radio System (TSRS) Solar Radio Event List


Purpose:
Trieste Solar Radio System decimetric event list
Description
Solar radio bursts at 1420 and 2695 MHz with flux density greater than 400 sfu (solar flux unit) have been analysed in order to characterise them in time, peak flux density, dominant circular polarization sense, and morphological class. The list contains events from 2000 to 2006. The morphological classification has been carried out based on the specifications illustrated in Solar-Geophysical Data, Explanation of data reports (July 1987, No. 515).
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Peak time of event.
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time of event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
freq MHz (1.0E+6>s-1)
Radio frequency of observation.
(UCD: em.freq;em.radio, UTYPE: helio:radio.frequency)
cpp percent (1.0>percent)
Circular polarization percentage measured at peak flux.
(UCD: phys.polarization.circular, UTYPE: helio:radio.circular_polarization_percent)
ps ()
Polarization sense (R - Right-handed; L - Left-handed).
(UCD: phys.polarization.circular, UTYPE: helio:radio.polarization_direction)
sfu_max sfu (1.0E-22>Wm-2Hz-1)
Maximum flux (solar flux units).
(UCD: phot.flux;stat.max, UTYPE: helio:radio.sfu_max)
radio_class ()
Morphological classification of the radio events based on Solar-Geophysical Data, Explanation of data reports (July 1987, No. 515) Morphological classes: SPIKE: Very fast and narrow event S 1: Simple and impulsive event with a narrow maximum region S 2: Simple and impulsive event with a wider maximum region C: Complex event: combination of a few or many simple bursts F: Fluctuation: minor C sometimes superposed in the main burst GB: Great Burst: particularly complex, long lasting event SER: Series of events occurring in a short time period Combinations of this symbols can be used for events not completely described by the previous classification classes.
(UCD: meta.code.class;em.radio, UTYPE: helio:radio.radio_class)
comment ()
Comments. Events that saturated the receiver are flagged as "SAT"(uration).
(UCD: meta.note, UTYPE: helio:comment)
data_url ()
URL link to quick-look picture file.
(UCD: meta.ref.url, UTYPE: helio:radio.data_url)

wind_typeii_soho_cme

Type II Radio Burst (WIND) and Associated CME (SOHO) List


Purpose:
List of Radio-loud CMEs observed by the Wind/WAVES experiment
Description
This is a catalog of type II bursts observed by the Radio and Plasma Wave (WAVES) experiment on board the Wind spacecraft and the associated coronal mass ejections (CMEs) observed by the Solar and Heliospheric Observatory (SOHO) mission. The type II burst catalog is derived from the Wind/WAVES catalog available at http://lep694.gsfc.nasa.gov/waves/waves.html by adding a few missing events. The CMEs in this catalog are called radio-loud CMEs because of their ability to produce type II radio bursts. The CME sources are also listed, as derived from the Solar Geophysical Data listing or from inner coronal images such as Yohkoh/SXT and SOHO/EIT. Some solar sources have also been obtained from Solarsoft Latest Events Archive after October 1, 2002: http://www.lmsal.com/solarsoft/latest_events_archive.html
Caveats
Acknowledgement/References
http://cdaw.gsfc.nasa.gov/CME_list/radio/waves_type2.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of the type II burst.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of the type II burst.
(UCD: time.end, UTYPE: helio:time_period.time_end)
freq_start s-1 (1.0>s-1)
Starting frequency of type II burst (kHz).
(UCD: em.freq, UTYPE: helio:radio.frequency_start)
freq_end s-1 (1.0>s-1)
Ending frequency of type II burst (kHz).
(UCD: em.freq, UTYPE: helio:radio.frequency_end)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic Latitude.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic Longitude.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of active region
(UCD: pos, UTYPE: helio:location.long_carr)
loc Unitless ()
Solar source location (Loc) of the associated eruption in heliographic coordinates. S25E16 means the latitude is 25 deg south and 16 deg east (source located in the southeast quadrant of the Sun. N denotes northern latitudes and W denotes western longitudes. Entries like SW90 indicate that the source information is not complete, but we can say that the eruption occurs on the west limb but at southern latitudes; if such entries have a subscript b (e.g., NE90b) it means that the source is behind the particular limb. This information is usually gathered from SOHO/EIT difference images, which show dimming above the limb in question. Completely backside events with no information on the source location are marked as BACK.
(UCD: pos.bodyrc;pos.heliographic, UTYPE: pos.bodyrc;pos.heliographic)
nar NAR # (1>Unitless)
NOAA active region index. If the active region number is not available or if the source region is not an active region, the entry is blank.
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
filar ()
Flag indicating set to either "FILA" for filament region or "DSF" for disappearing solar filament
(UCD: , UTYPE: )
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
time_cme UT (1.0>UT)
Time of the associated CME.
(UCD: time.start, UTYPE: cme.time_start)
pa degrees (1.0>degrees)
Central position angle for non-halo CMEs. (See the 'Central position angle' in the HEC glossary for the specification of this field)
(UCD: pos.posAng, UTYPE: helio:location.pa)
pa_width_ll ()
Flag ">" which indicates if the pa_width field is a lower limit, otherwise set to ""
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
pa_width degrees (1.0>degrees)
CME width in the sky plane. Width = 360 means the CME is a fill halo. For some entries, there is a prefix >, which means the reported width is a lower limit.
(UCD: pos.posAng;phys.angSize, UTYPE: helio:location.pa_width)
v_ps km s-1 (1.0E3>ms-1)
CME speed in the sky plane (km s-1).
(UCD: phys.veloc, UTYPE: helio:cme.velocity.v_plane_of_sky)
comment ()
Comments.
(UCD: meta.note, UTYPE: helio:comment)

ulysses_hxr_flare

Ulysses Catalog of Solar Hard X-Ray Flares


Purpose:
The catalogue of Solar Hard X-Ray Flares observed by Ulyssses GRB experiment.
Description
Ulysses was launched in October 1990, and its Solar X-ray/Cosmic Gamma-Ray Burst Experiment (GRB) has provided more than 13 years of uninterrupted observations of solar X-ray flare activity. Due to the large variation of the relative solar latitude and longitude of the spacecraft orbit with respect to the Earth, the perspective of the GRB instrument often differed significantly from that of X-ray instruments on Earth-orbiting satellites.
Caveats
Acknowledgement/References
Tranquille et al, 2009, Solar Physics, 258, p141.
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
The time that the start of the X-ray flare event was detected by Ulysses
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of the peak X-ray flux
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
The time that the X-ray event ends
(UCD: time.end, UTYPE: helio:time_period.time_end)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of x-ray flare from GOES location.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of x-ray flare from GOES location.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of x-ray flare from GOES location.
(UCD: pos, UTYPE: helio:location.long_carr)
xray_class X-ray class (1.0>(Wm-2 *10^[C=-6,M=-5,X=-4]))
mportance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
r_hci AU (1.496E+11>m)
Distance of Ulysses from the Sun (AU).
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: helio:location.r_hci)
lat_hci degrees (1.0>degrees)
Solar latitude.
(UCD: pos.bodyrc.lat;pos.heliocentric, UTYPE: helio:location.lat_hci)
long_hci degrees (1.0>degrees)
Solar longitude
(UCD: pos.bodyrc.long;pos.heliocentric, UTYPE: helio:location.long_err)
grb_incr ()
Indicates whether the flare is seen as a count rate increase in the Ulysses data (Y) or not (N), or whether it is not known (?) due to missing telemetry or to a high background caused by in situ charged particles.
(UCD: meta.code, UTYPE: )
fsu_angle degrees (1.0>degrees)
Flare-Sun-Ulysses (F-S-U) angle.
(UCD: pos.phaseAng, UTYPE: )
countrate_peak s-1 (1.0>s-1)
The peak count rate (non-normalized and corrected for rollover and dead time effects where necessary) measured by GRB during the event if seen.
(UCD: phys.energy;stat.max;meta.number, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)

ulysses_hxr_flare_farside

Ulysses Catalog of Solar Hard X-Ray Flares on the Far-side of the Sun


Purpose:
The catalogue of Solar flare X-ray events observed by the Ulysses GRB experiment not observed by GOES.
Description
The solar flare X-ray events in this list do not have an associated event observed by GOES and so are presumably on the far-side of the Sun. The list of these flares, providing the date and time of each event, together with the effective GOES X-ray class estimated using a scaling law given in the paper by Tranquille et al, 2009. The criteria used to identify these flares were a GRB intensity profile consistent with a solar flare event, a normalized peak count rate greater than a threshold value of 2 104 counts s_1 and the absence of any M- or X-class flare in the GOES event list.
Caveats
Acknowledgement/References
Tranquille et al, 2009, Solar Physics, 258, p141.
Parameters:
HEC_id HEC id (1.0>Unitless)
Event Identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
The time that the start of the X-ray flare event was detected by Ulysses.
(UCD: time.start, UTYPE: helio:time_period.time_start)
r_hci AU (1.496E+11>m)
Distance of Ulysses from the Sun (AU).
(UCD: pos.bodyrc.alt;pos.heliocentric, UTYPE: location.r_hci)
countrate_peak s-1 (1.0>s-1)
The non-normalized peak GRB count rate after correction for dead time and rollover.
(UCD: phys.energy;stat.max;meta.number, UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
inferred_xray_class X1 units (1.0E-4>Wm-2)
The inferred GOES X-class intensity.
(UCD: phot.flux; em.X-ray, UTYPE: )
xray_class_error X1 units (1.0E-4>Wm-2)
The Uncertainty in GOES X-class intensity.
(UCD: phot.flux;meta.code.error, UTYPE: )

ulysses_grb_xray_flare

Ulysses/GRB X-ray Flare List


Purpose:
A list of solar X-ray events deteced by the Gamma Ray Burst (GMB) experiment on Ulysses
Description
All the solar X-ray events detected by Ulysses GRB. In many cases the events were observed by other spacecraft. In some cases, however, a solar origin is inferred from the event time history.
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)

(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
The time the X-ray flare events were detected by Ulysses
(UCD: time.start, UTYPE: helio:time.time_start.insitu_time_start)
time_start_earth UT (1.0>UT)
The time the corresponding event was detected near the Earth by the GOES spacecraft.
(UCD: time.phase, UTYPE: helio:time.time_start.insitu_time_start)
r_hgi AU (1.496E+11>m)
The heliocentric distance of Ulysses at the time of the event.
(UCD: pos.distance;pos.heliocentric/heliographic?, UTYPE: helio:location.r_hgi)
lat_hgi degrees (1.0>degrees) HEEQ
The heliocentric latitude of Ulysses at the time of the event.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hgi)
long_hgi degrees (1>degrees) HEEQ
The heliocentric longitude of Ulysses at the time of the event.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hgi)

ulysses_swoops_icme

Ulysses/SWOOPS Interplanetary CME List


Purpose:
List of CMEs observed by the SWOOPS particle instrument on Ulysses.
Description
The Ulysses ICME list for the period from February 18, 1992 through April 5, 2008. The events from 1992 through 2002 were obtained directly from the Ulysses ICME list (http://swoops.lanl.gov/cme_list.html). The events from the start of 2003 onward were identified by Ebert et al (J. Geophys. Res., 114, 2009). The identification of ICMEs from in-situ solar wind measurements is not a straightforward process [Gosling, 1996; Zurbuchen and Richardson, 2006]. There is no single feature exhibited by all ICMEs and no standard signature that can be used to identify them all. A combination of signatures was used to find ICMEs in the SWOOPS and MAG data. These signatures include bi-directional electrons [Montgomery et al., 1974; Gosling et al., 1987], lower than expected proton temperature (Tp/Tex < 0.5) [Gosling et al., 1973], enhanced alpha/proton ratio (Na/Np > 0.08) [Borrini et al., 1982], enhanced magnetic field strength, low plasma beta (< 0.1), and smooth rotation in the magnetic field vector [Burlaga et al., 1981]. The expected proton temperature (Tex) was calculated using the Tp _ V relation from the Genesis mission [Neugebauer et al., 2003], which was derived from solar wind speed and temperature measurements from both the Genesis spacecraft and the SWEPAM instrument [McComas et al., 1998b] on the Advanced Composition Explorer (ACE) spacecraft. All ICME events were identified by eye using the signatures outlined above. In general, at least two signatures within a given solar wind interval were required before it was identified it as an ICME. It should be noted that owing to power limitations on the Ulysses spacecraft, the electron pitch angle distribution data used for identifying bi-directional electrons was unavailable from October 2004 through 25 March 2006 and available only intermittently after then. The Ulysses ICME list presented here covers a period that coincides with the declining phase of solar cycle 22 and all of solar cycle 23.
Caveats
Because of the nature of the Ulysses orbit, a nearly half (~49%) of these 178 events were observed at R > 5.0 AU. The maximum number of events in a single year (39) occurred in 1999, coinciding with the ascending phase of solar cycle 23, whereas only a single event was identified in the years 1995, 2006 and 2007. The latter were periods when Ulysses was embedded in the fast PCH flows, near solar minimum. Given that events were identified by eye, some smaller or less clear events may have been excluded from our survey.
Acknowledgement/References
http://swoops.lanl.gov/Ulysses-SWOOPSICMElist.doc
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
CME start time
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
CME end time.
(UCD: time.end, UTYPE: helio:time_period.time_end)
lat_hgi degrees (1.0>degrees)
The spacecraft heliographic inertial (HGI) latitude at the beginning of the event.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hgi)
long_hgi degrees (1.0>degrees)
The spacecraft heliographic inertial (HGI) longitude for the the day in which the event was identified.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hgi)
r_hgi AU (1.496E+11>m)
Ulysses-Sun radial distance using the heliographic inertial (HGI) coordinate system.
(UCD: pos.bodyrc.alt;pos.heliographic, UTYPE: helio:location.r_hgi)
v_p km s-1 (1.0E3>ms-1)
Average proton velocity within the event timeframe.
(UCD: phys.veloc, UTYPE: helio:icme.velocity.v_proton)
v_p_err km s-1 (1.0E3>ms-1)
Error in the average proton velocity.
(UCD: phys.veloc;stat.error, UTYPE: helio:icme.velocity.v_uncertainty_factor)
b nT (1.0E-9>T)
Average total magnetic field strength of the plasma within the event timeframe.
(UCD: phys.magField;stat.mean, UTYPE: helio:icme.plasma_magnetic_field_strength)
b_err nT (1.0E-9>T)
Error in the magnetic field strength.
(UCD: stat.error;phys.magField, UTYPE: helio:icme.plasma_magnetic_field_strength_error)

wind_ace_sir

Wind and ACE List SIRs List


Purpose:
Stream Interactions Regions (SIRs) from Wind and ACE Data.
Description
The Stream Interaction Regions (SIRs) are identified based on an inspection of the following features: an increase of solar wind speed, a pile-up of total perpendicular pressure (Pt) with gradual decreases at both sides from the Pt peak to the edges of the interaction region, velocity deflections, an increase of proton number density, an enhancement of proton temperature, an increase of entropy, a compression of magnetic field. The presence of at least 5 signatures is required, and SIRs are identified with careful consideration of the ambient solar wind. In order to survey the SIRs as completely as possible, ACE data have been used when the Wind data were unavailable or noisy and when Wind was near or within the magnetosphere. The SIRs include corotating interaction regions (CIRs) and tranisent stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycles.
Caveats
Jian et al. (Solar Physics, 2006, 239, 337) gives more details about the identification criteria and also the SIR list of 1995 _ 2004. The SIR list of 1995 _ 2006 is an appendix of Lan Jian's 2008 PhD thesis. Jian et al. (Solar Physics, WHI special issue, 2011, in press) updates the results to 2009.
Acknowledgement/References
Jian et al. (Solar Physics, WHI special issue, 2011, in press)
Parameters:
HEC_id HEC id (1>Unitless)
Event Identification number (HEC internal number).
(UCD: meta.record, UTYPE: )
sir_id Unitless (1>Unitless)
Stream interaction region number which is reset to 1 at the beginning of the year.
(UCD: meta.id, UTYPE: )
flag_hybrid ()
* means that it is a hybrid case consisting of more than one event.
(UCD: meta.code, UTYPE: )
cir_id Unitless (1>Unitless)
Corotating interaction region (CIR) number which is reset to 1 at the beginning of the year.
(UCD: meta.id, UTYPE: )
time_start UT (1.0>Unitless)
Start time of the event.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>Unitless)
End time of the event.
(UCD: time.end, UTYPE: helio:time_period.time_end)
time_discon1 UT (1.0>Unitless)
Time of the first discontinuity.
(UCD: time.epoch, UTYPE: )
f_r_shock1 ()
If there is a dicontinuity, this has one of the following values: F it is a forward shock, R it is a reverse shock, / it is neither a forward or a reverse shock, SR it is a slow reverse shock, from Justin Kasper's shock list of Wind.
(UCD: meta.code, UTYPE: )
time_discon2 UT (1.0>Unitless)
Time of the second discontinuity.
(UCD: time.epoch, UTYPE: )
f_r_shock2 ()
If there is a second dicontinuity, this has one of the following values: F it is a forward shock, R it is a reverse shock, / it is neither a forward or a reverse shock, SR it is a slow reverse shock, from Justin Kasper's shock list of Wind.
(UCD: meta.code, UTYPE: )
time_discon3 UT (1.0>Unitless)
Time of the third discontinuity.
(UCD: time.epoch, UTYPE: )
f_r_shock3 ()
If there is a third dicontinuity, this has one of the following values: F it is a forward shock, R it is a reverse shock, / it is neither a forward or a reverse shock, SR it is a slow reverse shock, from Justin Kasper's shock list of Wind.
(UCD: meta.code, UTYPE: )
time_si UT (1.0>Unitless)
Time at the stream interface.
(UCD: time.epoch, UTYPE: )
pt_max pPa (1.0E-12>kgm-1.s-2)
Maximum total perpendicular pressure.
(UCD: phys.pressure;stat.max, UTYPE: )
v_max km.s-1 (1000>m.s-1)
Maximum velocity.
(UCD: phys.veloc;stat.max, UTYPE: )
v_min km.s-1 (1000>m.s-1)
Minimum velocity.
(UCD: phys.veloc;stat.min, UTYPE: )
delta_v km.s-1 (1000>m.s-1)
Difference between maximum and minimum velocities.
(UCD: arith.rate;phys.veloc, UTYPE: )
b_max nT (1.0E-9>Tesla)
Peak magnetic field intensity.
(UCD: stat.max;phys.magField, UTYPE: )
comment ()
Comments.
(UCD: meta.note, UTYPE: helio:comment)

wind_stereo_ii_iv_radioburst

WIND and STEREO Candidate Type II and IV Radio Burst List


Purpose:
WAVES Experiment on WIND and STEREO - Type II/IV List
Description
This is a listing year-by-year of POSSIBLE solar type II and type IV bursts detected by the WAVES instruments on the Wind and STEREO spacecraft. Each table entry consists of a start and stop time and an upper and lower frequency limit. The four items form a box on the dynamic spectrum which contains the bursts. It is not always the case that the highest (lowest) frequency happens at the earliest (latest) time. Also included in most entries are comments and a dynamic spectrum of at least part of the emission. The dynamic spectra come in two flavors: those marked with 'S' or 'X' are standard frequency versus time dynamic spectra. Those marked with 'F' are inverse frequency versus time, corresponding roughly to distance from the sun versus time.
Caveats
Acknowledgement/References
http://lep694.gsfc.nasa.gov/waves/
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
identifier (1>Unitless)
An internal WAVES Experiment Type II/IV event identifier, which, as the events are organised in separate files for each year, is incremented for each event during the year and reset to 1 at the start of the next year.
(UCD: meta.id.cross, UTYPE: helio:external_reference_id)
time_start UT (1.0>UT)
Start time of radio burst.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time of radio burst.
(UCD: time.end, UTYPE: helio:time_period.time_end)
freq_start s-1 (1.0>s-1)
Start of frequency range measured.
(UCD: em.freq, UTYPE: helio:radio.frequency_start)
freq_end s-1 (1.0>s-1)
End of frequency range measured.
(UCD: em.freq, UTYPE: helio:radio.frequency_end)
dyn_spec ()
Dynamic spectra type: Those marked with 'S' or 'X' are standard frequency versus time dynamic spectra. Those marked with 'F' are inverse frequency versus time, corresponding roughly to distance from the sun versus time.
(UCD: meta.code, UTYPE: helio:radio.dyn_spectra)
comment ()
Comments -brief description of type of burst.
(UCD: meta.note, UTYPE: helio:comment)

wind_mfi_bs_crossing_time

WIND/MFI Bow Shock Cross Crossing Time List


Purpose:
List of WIND MFI Bow Shock crossing times
Description
The Bow Shock is the shock wave observed just upstream of the Earth's magnetosphere caused by the supersonic and super-Alfvenic solar wind ramming into the Earth's magnetosphere. (SuperAlfvenic refers to when the solar wind's speed exceeds a characteristic speed that depends on the solar wind's density and the interplanetary magnetic field strength.) The MFI team has provided a list of all WIND bow shock crossings. The event list provides a list of bow shock (BS) crossing times. For each crossing, the following times are given: The time of the last BS crossing as the spacecraft was leaving the Earth magnetosheath. The first full hour which has only unshocked solar wind data in it. The last full hour which still contains interplanetary magnetic field data. The time of the 1st BS crossing on the way into the Earth magnetosphere.
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
last_bs_crossing UT (1.0>UT)
The time of the last BS crossing as the spacecraft was leaving the Earth's magnetosheath.
(UCD: time.phase, UTYPE: )
flag_last_bs ()
A flag to indicate one of the following for the last BS crossing time: #: First data point in our data set *: BS occurred in data gap, time listed is the last point before the gap +: Strong foreshock activity before BS also excluded
(UCD: meta.code, UTYPE: )
first_hr_kept UT (1.0>UT)
The first full hour which has only unshocked solar wind data in it.
(UCD: time.phase, UTYPE: )
flag_first_hr ()
A flag to indicate one of the following for the last BS crossing time: +: Strong foreshock activity before BS also excluded
(UCD: meta.code, UTYPE: )
last_hr_kept UT (1.0>UT)
The last full hour which still contains interplanetary magnetic field data.
(UCD: time.phase, UTYPE: )
flag_last_hr ()
A flag to indicate one of the following for the last BS crossing time: +: Strong foreshock activity before BS also excluded
(UCD: meta.code, UTYPE: )
first_bs_crossing UT (1.0>UT)
The time of the 1st BS crossing on the way into the Earth magnetosphere.
(UCD: time.phase, UTYPE: )
flag_first_bs ()
A flag to indicate one of the following for the last BS crossing time: #: First data point in our data set *: BS occurred in data gap, time listed is the last point before the gap +: Strong foreshock activity before BS also excluded
(UCD: meta.code, UTYPE: )
time_start UT (1.0>UT)
Start time set as the last BS crossing time.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
End time set as the time of the 1st BS crossing on the way into the Earth magnetosphere.
(UCD: time.end, UTYPE: helio:time_period.time_end)

wind_mfi_ip_shock

WIND/MFI Interplanetary Shock List


Purpose:
List of Interplanetary Shocks identified by the WIND MFI instrument.
Description
This list contains the times of interplanetary shocks identified by the WIND MFI instrument. (Note that there was provision for the type of shock and driver in the list, but these fields have no data so the list only contains times.)
Caveats
Acknowledgement/References
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of shock.
(UCD: time.start, UTYPE: helio:time_period.time_start)

wind_mfi_mag_cloud

WIND/MFI Magnetic Cloud List


Purpose:
List of Magnetic Cloud events observed by the WIND MFI instrument.
Description
A magnetic cloud is a transient ejection in the solar wind defined by relatively strong magnetic fields, a large and smooth rotation of the magnetic field direction over approximately 0.25AU at 1AU, and a low proton temperature [Burlaga et al., 1981]. Magnetic clouds are ideal objects for solar-terrestrial studies because of their simplicity and their extended intervals of southward and northward magnetic fields [Burlaga et al., 1990] The table consists of estimated start and end times that were estimated by a magnetic field model [Lepping et al., 1990] that assumes that the field within the magnetic cloud is force free, i.e., so that the electrical current and the magnetic field are parallel and proportional in strength everywhere within its volume.
Caveats
Acknowledgement/References
http://wind.nasa.gov/mfi/mag_cloud_pub1.html#table
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Estimated start time of magnetic cloud (using the magnetic field model of Lepping et al., 1990). .
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
Estimated end time of the magnetic cloud (using the magnetic field model of Lepping et al., 1990).
(UCD: time.end, UTYPE: helio:time_period.time_end)
code ()
Code number for identification.
(UCD: meta.id, UTYPE: helio:solar_wind.magnetic_cloud_id)
quality Unitless (1.0>Unitless)
Quality: 1 = Excellent, 2 = Good, 3 = Poor
(UCD: meta.code.class, UTYPE: helio:solar_wind.magnetic_cloud_quality)

yohkoh_sxt_trace_list

YOHKOH SXT TRACE flare list


Purpose:
Common flares observed by Yohkoh/SXT and TRACE.
Description
This list is compiled from the Yohkoh flare directories at ISAS as maintained by Mr. Sawa and the online TRACE catalog generated by SSW. In the following table, click a line under 'SXT PFI file' (leftmost column) for a plot of GOES/HXT light curves and SXT/TRACE data coverage.
Caveats
Acknowledgement/References
http://www.lmsal.com/nitta/sxt_trace_flares/list.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
link ()
Link to the SXT PFI file at ISAS.
(UCD: meta.ref.url, UTYPE: )
time_start_sxt UT (1.0>UT)
Time of first flare mode SXT image.
(UCD: time.start, UTYPE: )
time_end_sxt UT (1.0>UT)
Time of last flare mode SXT image.
(UCD: time.start, UTYPE: )
xray_class ()
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
n_img Unitless (1>Unitless)
Number of flare mode SXT images.
(UCD: meta.number, UTYPE: )
x_arcsec_sxt arcsec (2.7778E-4>degrees)
X coordinate (in arcsec from disk center) of the center of the 6th SXT flare mode image. Picked up the 6th because SXT sometimes changes the field of view after the first flare mode image.
(UCD: pos.cartesian.x;pos.bodyrc;pos.heliographic/heliocentric, UTYPE: )
y_arcsec_sxt arcsec (2.7778E-4>degrees)
Y coordinate (in arcsec from disk center) of the center of the 6th SXT flare mode image. Picked up the 6th because SXT sometimes changes the field of view after the first flare mode image.
(UCD: pos.cartesian.y;pos.bodyrc;pos.heliographic/heliocentric, UTYPE: )
time_start UT (1.0>UT)
First TRACE image in the period (time_start_sxt - 30min, time_end_sxt + 30min).
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_end UT (1.0>UT)
Last TRACE image in the period (time_start_sxt - 30min, time_end_sxt + 30min).
(UCD: time.end, UTYPE: helio:time_period.time_end)
time_sxt_trace UT (1.0>UT)
Time of the TRACE image closest to time_start_sxt.
(UCD: time.creation, UTYPE: )
wl_dom Angstrom (1.0E-10>m)
Wavelength at which the greatest number of TRACE images is taken.
(UCD: em.wl, UTYPE: )
x_arcsec arcsec (2.7778E-4>degrees)
X coordinate (in arcsec from disk center) of the center of the TRACE image at time_sxt_trace.
(UCD: pos.cartesian.x;pos.bodyrc;pos.heliographic/heliocentric, UTYPE: )
y_arcsec arcsec (2.7778E-4>degrees)
Y coordinate (in arcsec from disk center) of the center of the TRACE image at time_sxt_trace.
(UCD: pos.cartesian.y;pos.bodyrc;pos.heliographic/heliocentric, UTYPE: )
n171 Unitless (1>Unitless)
Number of TRACE images at 171 Angstroms.
(UCD: meta.number;em.wl;em.UV.10-50nm, UTYPE: )
n195 Unitless (1>Unitless)
Number of TRACE images at 195 Angstroms.
(UCD: meta.number;em.wl;em.UV.10-50nm, UTYPE: )
n284 Unitless (1>Unitless)
Number of TRACE images at 284 Angstroms.
(UCD: meta.number;em.wl;em.UV.10-50nm, UTYPE: )
n1600 Unitless (1>Unitless)
Number of TRACE images at 1600 Angstroms.
(UCD: meta.number;em.wl;em.UV.100-200nm, UTYPE: )
n1216 Unitless (1>Unitless)
Number of TRACE images at 1216 Angstroms.
(UCD: meta.number;em.wl;em.UV.100-200nm, UTYPE: )
nwl Unitless (1>Unitless)
Number of TRACE White Light images.
(UCD: meta.number;em.wl;em.opt, UTYPE: )

yohkoh_hxr_flare

Yohkoh/HXT Hard X-ray Flare List


Purpose:
Flare list from the Yohkoh Hard X-ray Telescope
Description
This list contains all solar flares recorded with Yohkoh HXT during the interval be- tween October 1, 1991 and December 14, 2001. The HXT is a hard X-ray imager of the Fourier-synthesis type, consisting of 64 mod- ulation subcollimators. Each modulation subcollimator is equipped with a small NaI(Tl) scintillator and photomultiplier tube, and measures a modulated photon count. A set of the 64 photon counts, transmitted from the satellite to the ground, is converted into an image by image synthesis procedures. The main characteristics of HXT are summarized below: i) Simultaneous imaging in four energy bands, namely, the L-band (13.9 - 22.7 keV), M1-band (22.7 - 32.7 keV), M2-band (32.7 - 52.7 keV), and H-band (52.7 - 92.8 keV). Ii) Angular resolution of about 5 arcsec with a wide field of view covering the whole Sun. Iii) Basic temporal resolution of 0.5 s. Iv) High sensitivity with an effective area of about 60 cm2. The events in the list also include the position of the X-ray flare and the Wide Band Spectrometer (WBS) data provided in the electronic supplementary material to the paper of Sato et al, 2006, Solar Physics, 236, p351.
Caveats
Note that due to orbit there is not 24 hour coverage. In the Yohkoh operation, the observation mode is automatically controlled by the onboard Data Processor, and intense flares trigger the so-called Flare mode. Weak fl ares, however, are recorded in the Quiet mode without triggering the Flare mode. Since only the L-band count rate is recorded in the Quiet mode, flares sometimes lack the M1-, M2-, and H-band count rates.
Acknowledgement/References
http://gedas22.stelab.nagoya-u.ac.jp/HXT/catalogue/image_html/all_images.html
Parameters:
HEC_id HEC id (1>Unitless)
Event identification number (HEC internal number)
(UCD: meta.record, UTYPE: )
time_start UT (1.0>UT)
Start time of flare.
(UCD: time.start, UTYPE: helio:time_period.time_start)
time_peak UT (1.0>UT)
Time of flare maximum.
(UCD: time.phase, UTYPE: helio:time.time_peak)
time_end UT (1.0>UT)
End time of flare.
(UCD: time.end, UTYPE: helio:time_period.time_end)
nar NAR # (1>Unitless)
NOAA active region index
(UCD: meta.id.cross, UTYPE: helio:flare.nar)
lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of H-alpha flare.
(UCD: pos.bodyrc.lat;pos.heliographic, UTYPE: helio:location.lat_hg)
long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of H-alpha flare.
(UCD: pos.bodyrc.long;pos.heliographic, UTYPE: helio:location.long_hg)
long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of H-alpha flare.
(UCD: pos, UTYPE: helio:location.long_carr)
xray_class ()
Importance of flare at X-ray wavelengths -- the peak flux measured at Earth in the 0.1 to 0.8 nm range in units of W m-2. (See the 'X-ray Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.X-ray, UTYPE: helio:flare.magnitude.xray_class)
optical_class ()
Average optical importance of flare -- a measurement of flare size and brilliance. (See the 'Optical Class' in the HEC glossary for the specification of this field)
(UCD: meta.code.class;em.opt, UTYPE: helio:flare.magnitude.optical_class)
hxt_lo Unitless (1>Unitless)
L-band (13.9 - 22.7 keV) peak count rate in cts s-1 SC-1 (with background of ~ 2 cts s-1 SC-1)
(UCD: , UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
hxt_m1 Unitless (1>Unitless)
M1-band (22.7 - 32.7 keV) peak count rate in cts s-1 SC-1 (with background of ~ 1 cts s-1 SC-1)
(UCD: , UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
hxt_m2 Unitless (1>Unitless)
M2-band (32.7 - 52.7 keV) peak count rate in cts s-1 SC-1 (with background of ~ 1 cts s-1 SC-1).
(UCD: , UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
hxt_hi Unitless (1>Unitless)
H-band (52.7 - 92.8 keV) peak count rate in cts s-1 SC-1 (with background of ~ 9 cts s-1 SC-1).
(UCD: , UTYPE: helio:flare.magnitude.hard_xray_quantifier.hard_xray_count)
sxs_pc21 cts.s-1 (1.0>s-1)
3 - 30 keV peak count rate in cts s-1.
(UCD: , UTYPE: )
sxs_pc22 cts.s-1 (1.0>s-1)
3 - 30 keV peak count rate in cts s-1.
(UCD: , UTYPE: )
hxs_pc1 cts.s-1 (1.0>s-1)
20 - 50 keV peak count rate in cts s-1.
(UCD: , UTYPE: )
hxs_pc2 cts.s-1 (1.0>s-1)
50 - 600 keV peak count rate in cts s-1.
(UCD: , UTYPE: )
x_lat_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic latitude of X-ray flare.
(UCD: , UTYPE: )
x_long_hg degrees (1.0>degrees) Stonyhurst Heliographic
Heliographic longitude of X-ray flare.
(UCD: , UTYPE: )
x_long_carr degrees (1.0>degrees) Carrington Heliographic
Carrington longitude of X-ray flare.
(UCD: , UTYPE: )
comment ()
Comments
(UCD: meta.note, UTYPE: helio:comment)
yoh_event Untiless (1>Untiless)
Yohkoh HXT event number.
(UCD: , UTYPE: )