CME - FLARE - Dst - FD test 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 prior to 2011 were taken from SPIDR: http://spidr.ngdc.noaa.gov/spidr/ Forbush decrease data after 2011 were taken from NEST: http://previ.obspm.fr/hidden3/search.php *** 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) v (kmps): the linear speed obtained by linear (first-order polynomial) fit to the height-time measurements WIDTH (deg): The sky-plane width of CMEs (typically measured in the C2 FOV after the width becomes stable) ******************************************************************************************************************************************************************** SOLAR FLARE PARAMETERS ******************************************************************************************************************************************************************** position: 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 r (Rsun): distance from the center of the solar disc in Rsun X-ray class: according to the order of magnitude of the peak burst intensity (B,C,M or X) X-ray I: a number from 1.0 to 9.9 that multiplies the X-ray class X-ray peak I (W/m2): magnitude of the peak burst intensity ******************************************************************************************************************************************************************** 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 ******************************************************************************************************************************************************************** Dst PARAMETERS ******************************************************************************************************************************************************************** Dst measurement time: time of measured Dst minimum |Dst| (nT): absolute value of the minimum of Dst, measured from Dst value at the onset ******************************************************************************************************************************************************************** comment: observer's comment on whether or not CME hit or missed the Earth ******************************************************************************************************************************************************************** FORBUSH DECREASE PARAMETERS ******************************************************************************************************************************************************************** |FD|(%): Forbush decrease magnitude (absolute value of the decrease, measured from the onset time to minimum)