| Parameters | |||
| name: | hec_id | ||
| datatype: | int | ucd: | meta.record |
| xtype: | utype: | ||
| description: | Event Identification number (HEC internal number). | ||
| name: | time_start | ||
| datatype: | char | ucd: | time.start |
| xtype: | iso8601 | utype: | helio:time_period.time_start |
| description: | Start time of the event. | ||
| name: | time_peak | ||
| datatype: | char | ucd: | time.phase |
| xtype: | iso8601 | utype: | time.time_peak |
| description: | Time of the peak of the event. | ||
| name: | time_end | ||
| datatype: | char | ucd: | time.end |
| xtype: | iso8601 | utype: | helio:time_period.time_end |
| description: | End time of event. | ||
| name: | loc_source | ||
| datatype: | char | ucd: | meta.code;pos |
| xtype: | utype: | ||
| description: | 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. | ||
| name: | lat_hg | ||
| datatype: | float | ucd: | pos.bodyrc.lat;pos.heliographic |
| xtype: | utype: | location.lat_hg | |
| description: | Heliographic latitude of x-ray flare. | ||
| name: | long_hg | ||
| datatype: | float | ucd: | pos.bodyrc.long;pos.heliographic |
| xtype: | utype: | location.long_hg | |
| description: | Heliographic longitude of x-ray flare. | ||
| name: | long_carr | ||
| datatype: | float | ucd: | |
| xtype: | utype: | location.long_carr | |
| description: | Carrington longitude of x-ray flare. | ||
| name: | optical_class | ||
| datatype: | char | ucd: | meta.code.class;em.opt |
| xtype: | utype: | flare.magnitude.optical_class | |
| description: | 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) | ||
| name: | xray_class | ||
| datatype: | char | ucd: | meta.code.class;em.X-ray |
| xtype: | utype: | flare.magnitude.xray_class | |
| description: | 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) | ||
| name: | time_start_rise_sep | ||
| datatype: | char | ucd: | time.epoch |
| xtype: | iso8601 | utype: | |
| description: | Time at which the proton intensity starts to rise. | ||
| name: | upper_limit | ||
| datatype: | char | ucd: | meta.code;stat.max |
| xtype: | utype: | ||
| description: | Y if the peak integral proton intensity is an upper limit - N if not. | ||
| name: | intensity_sep_peak | ||
| datatype: | float | ucd: | stat.max;prot.flux |
| xtype: | utype: | ||
| description: | The peak integral proton intensity at energies above 10 MeV. | ||
| name: | intensity_sep_exp | ||
| datatype: | float | ucd: | prot.flux |
| xtype: | utype: | proton_event.proton_flux | |
| description: | 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. | ||
| name: | comment | ||
| datatype: | char | ucd: | meta.note |
| xtype: | utype: | ||
| description: | 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 â(c')â. (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 â(d')â). (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. | ||
Extracted from VOTable generated by HEC HQI on: 07-Sep-17 18:38:21