CME - FLARE - Dst - FD training list (1996 - 2011) ******************************************************************************************************************************************************************** Generated by HVAR Observatory, University of Zagreb Correspondence: mdumbovic@geof.hr ******************************************************************************************************************************************************************** CME key parameters are taken from the LASCO/SOHO catalog at: http://cdaw.gsfc.nasa.gov/CME_list/ For the full explanation of CME key parameters see: http://cdaw.gsfc.nasa.gov/CME_list/catalog_description.htm *** Solar flare key parameters were taken from the NOAA X-ray flare list at: ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SOLAR_FLARES/FLARES_XRAY/ For the full explanation of solar flare key parameters see: ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SOLAR_FLARES/FLARES_XRAY/docs/xray.fmt.REVISED *** CMEs were associated to solar flares using temporal and spatial criteria (using automatic method by Davor Sudar, D.S.). For the details see: B. Vršnak, D. Sudar, D. Ruždjak (2005), A&A 435 (3) 1149-1157 DOI: 10.1051/0004-6361:20042166 Several HALO CMEs were associated to flares by LASCO catalog team, data available at: http://cdaw.gsfc.nasa.gov/CME_list/halo/halo.html *** cross-cheking was made with CME-ICME-Dst list in Richardson & Cane (2010), available at: http://www.srl.caltech.edu/ACE/ASC/DATA/level3/icmetable2.htm for events not found in (R&C list) in-situ cross-cheking was made using magnetic field and solar wind data from ACE & WIND satellites, available at: http://www.srl.caltech.edu/ACE/ASC/level2/lvl2DATA_MAG-SWEPAM.html http://wind.gsfc.nasa.gov/mfi_swe_plot.php *** Forbush decrease data were taken from SPIDR: http://spidr.ngdc.noaa.gov/spidr/ *** for detailed explanation see: Dumbovic, M.; Devos, A.; Vrsnak, B.; Sudar, D.; Rodriguez, L.; Ruzdjak, D.; Leer, K.; Vennerstrom, S.; Veronig, A., 2015, "Geoeffectiveness of Coronal Mass Ejections in the SOHO Era" Dumbovic, M.; Vrsnak, B.; Calogovic, J., 2015, "Forbush decrease prediction based on the remote solar observations" ******************************************************************************************************************************************************************** CME PARAMETERS ******************************************************************************************************************************************************************** First C2 appearance: the date and time of first appearance in the LASCO/C2 field of view (FOV) (serves as an ID for each CME) CME start time: the CME onset time obtained by extrapolating the linear fit to the solar surface (height = 1 solar radius) N: number of measurements in height/time plot MPA (deg): the Measurement Position Angle, the position angle at which the height-time measurements are made CPA (deg): the Central Position Angle (some CMEs move nonradially so the CPA and MPA do not coincide) WIDTH (deg): The sky-plane width of CMEs (typically measured in the C2 FOV after the width becomes stable) v (kmps): the linear speed obtained by linear (first-order polynomial) fit to the height-time measurements h_beg (Rsun): the position of first measurement in height/time plot h_end (Rsun): the position of the last measurement in height/time plot (Rsun): the mean value between h_beg and h_end feat_qual: 1st quality index (by observer’s remark), 0.5 (ill defined) - 3 (excellent) QI: 2nd quality index (by observer’s remark), 0 (ill defined) - 5 (excellent) Remark: observer’s remark on the quality of observation/measurement (Ill-defined(Ill), poor, fair, typical(Typ), good & excellent(Exc)) Halo: 1 if halo (width=360 deg), 2 if partial halo (width>120 deg), 0 if width<120 Mass: Estimation of CME mass (very uncertain, should be taken as representative) Energy: Estimation of CME kinetic energy (obtained from the linear speed and the representative mass) ******************************************************************************************************************************************************************** SOLAR FLARE PARAMETERS ******************************************************************************************************************************************************************** Flare association: D.S. for automatic association, lasco for LASCO team association Flare start time: the time when the flux starts to rise Flare max time: the time when the flux value reaches maximum Flare end time: the time when the current flux reading returns to 1/2 the peak FDC (deg): Flare Distance from Center, angular distance of the flare position from the center of the solar disc (0 (center) < FDC < 90 (limb)) FPA (deg): Flare Position Angle, measured clockwise from the north (0 < FPA < 360) r (Rsun): distance from the center of the solar disc in Rsun Source region: the position of the flare in latitude and longitude, N or S for north or south latitude, E or W for east or west central meridian distance X-ray class: according to the order of magnitude of the peak burst intensity (B,C,M or X) X-ray intensity: a number from 1.0 to 9.9 that multiplies the X-ray class Peak: magnitude of the peak burst intensity Integrated Flux: the integrated flux from event start to end (beginning with January 1997 data) ******************************************************************************************************************************************************************** in-situ remark: the results of cross-checking with in-situ data and CME-ICME-Dst list in Richardson & Cane(2010) 1 matching event found in R&C list 2 event found in R&C list, R&C associate only one of the CMEs within a train 3 not in R&C list, but ICME signature found in in-situ data 4 event found in R&C list, but they associate different CME, or different Dst 5 no event in either R&C list, or in-situ data (CME missed the Earth) 6 no event in R&C list, in-situ data show high speed stream or complex event (ICME signature not obvious) 7 no event in R&C list, in-situ data gap on both ACE & WIND ******************************************************************************************************************************************************************** Dst PARAMETERS ******************************************************************************************************************************************************************** Dst measurement time: time of measured Dst minimum Dst minimum: minimum of Dst, measured from Dst=0 nT Dst relative minimum: minimum of Dst, measured from Dst value at the onset ******************************************************************************************************************************************************************** CME solo(S) / train(T): a note regarding possible CME-CME interactions, based on the source location of involved CMEs, the time of their liftoff and speed, 4 categories: S CME does not interact with other CMEs S? CME could interact with other CMEs, but most likely did not T? CME could interact with other CMEs and most likely did T CME interacted with other CMEs ******************************************************************************************************************************************************************** FORBUSH DECREASE PARAMETERS ******************************************************************************************************************************************************************** |FD|(%): Forbush decrease magnitude (absolute value of the decrease, measured from the onset time to minimum)