| 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: | Date. | ||
| name: | radio_10cm | ||
| datatype: | int | ucd: | phot.flux;em.radio.1500-3000MHz |
| xtype: | utype: | ||
| description: | Radio Flux Penticton 10.7 cm: The 10.7 cm (2800 MHz) full Sun radio flux reported by the Dominion Radio Astrophysical Observatory at Penticton, B.C., Canada on the date indicated. Measurements are made at approximately 2000UT. Values are in units of 10 E-22/Sq Wm/Hz and are not corrected for the variable Sun-Earth distance resulting from the eccentric orbit of the Earth around the Sun. | ||
| name: | sesc_ssn | ||
| datatype: | int | ucd: | meta.number;meta.modelled |
| xtype: | utype: | ||
| description: | Sunspot No: The SESC sunspot number for the indicated date is from the daily Solar Region Summary issued by SESC. The SESC sunspot number is computed according to the Wolf Sunspot Number R=k (10g+s), where g is the number of sunspot groups (regions), s is the total number of individual spots in all the groups, and k is a variable scaling factor (usually less than 1) that indicates the combined effects of observing conditions, telescope, and bias of the solar observers. A sunspot number of zero indicates there were no visible sunspots on that date; a * indicates that no observations were taken. The sunspot region information used to compute the daily sunspot number incorporates reports from as many as six observatories. These reports are used to form a composite picture of each individual region, including sunspot number, area and classification, taking into account such factors as the time of observation and the quality of seeing. This composite information is the daily average obtained from the reporting observatories and may not represent the latest data. It is reported daily in the Solar Region Summary and listed in the Region Summary section of the Weekly. | ||
| name: | ss_area | ||
| datatype: | int | ucd: | phys.area |
| xtype: | utype: | ||
| description: | Sunspot Area : Sum of the corrected area of all observed sunspots, in units of millionths of the solar hemisphere. | ||
| name: | new_regions | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | New Regions. | ||
| name: | stan_smf | ||
| datatype: | int | ucd: | |
| xtype: | utype: | ||
| description: | Stanford Solar Mean Field. | ||
| name: | xray_bkg | ||
| datatype: | char | ucd: | instr.background;phot.flux;em.X-ray;meta.code.class |
| xtype: | utype: | ||
| description: | X-ray Background Flux : The daily average background x-ray flux as measured on the SWPC primary GOES satellite. Note: X-ray flux values below the B1 level can be erroneous. Energetic electron contamination of the x-ray sensors occurs. At times of high electron flux at geosynchronous altitude, the x-ray measurementsin the low A-class range can be in error by 20-30%. Measurements taken duringperiods of low energetic electron fluxes are much more accurate. Daily GOES X-ray Background Flux algorithm: o The 24 one-hour X-ray 1-8 Angstrom; values are divided into three 8-hour sections o The minimum for each of these three 8-hour sections is determined; ... Call them min1, min2, and min3 o The average of the minima from the first and last 8-hour sections is calculated: min_avg = 1/2 (min1 + min3) o Daily Background X-Ray Flux is the smallest of min2 or min_avg X-Ray_background = minimum of (min2 or min_avg) | ||
| name: | n_c_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type C X-Ray Flares. | ||
| name: | m_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type M X-Ray Flares. | ||
| name: | x_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type X X-Ray Flares. | ||
| name: | opts_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type S Optical Flares. | ||
| name: | opt1_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type 1 Optical Flares. | ||
| name: | opt2_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type 2 Optical Flares. | ||
| name: | opt3_flares | ||
| datatype: | int | ucd: | meta.number |
| xtype: | utype: | ||
| description: | Number of Type 3 Optical Flares. | ||
Extracted from VOTable generated by HEC HQI on: 07-Sep-17 18:38:07