SOHO/MDI-Debrecen Data and SDO/HMI-Debrecen Data : NOAA - NOAA sunspot group number Proj. U - Projected umbra area in millionths of solar disc, negative values indicate that the umbra consists of fragmented regions which cannot be separated without losing umbral area. In this way several spots (intensity minima in the umbra) have a common umbra, e.g. -2 means that the given spot shares an umbra with spot No.2, and the common U value is indicated at spot No.2. Proj. U+P - Projected umbra + penumbra area in millionths of solar disc, negative values indicate that several umbras have a common penumbra, e.g. -7 means that the given umbra shares a penumbra with umbra No.7, and the U+P value is indicated at No.7. Corr. U - Corrected umbra area in millionths of solar hemisphere, for negative values see above Corr. U+P - Corrected umbra + penumbra area in millionths of solar hemisphere, for negative values see above B - Heliographic latitude B; positive: North, negative: South L - Heliographic longitude L LCM - Longitudinal distance from the Sun's central meridian Pos. angle - Position angle r - Distance from the centre of Sun's disc in terms of Sun's radius MU - Mean magnetic field within the umbra contour averaged the pixel values with sign. MP - Mean magnetic field within the penumbra contour averaged the pixel values with sign. Reuven Ramaty High Energy Solar Spectroscopic Imager Data: Flare - An ID number, ymmddnn, e.g., 2042101 is the first flare found for 21-Apr-2002. These numbers are not time ordered. Date - The date when the flare occurred Start - Flare start time Peak - Flare peak time End - Flare end time Dur[s] - Duration of flare in seconds Peak[c/s] - Peak count rate in corrected counts, peak counts/second Total Counts - Total of counts in corrected counts, counts in energy range Energy [keV] - The highest energy band in which the flare was observed. X pos [asec] - Flare position in arcsec from sun center Y pos [asec] - Flare position in arcsec from sun center Radial [asec] - Radial distance in arcsec from sun center B [deg] - Heliographic latitude B; positive: North, negative: South (this value is calculated, not in RHESSI data originally) L [deg] - Heliographic longitude L (this value is calculated, not in RHESSI data originally) Flags - Quality Codes Flare Flag Codes: a0 - In attenuator state 0 (None) sometime during flare a1 - In attenuator state 1 (Thin) sometime during flare a2 - In attenuator state 2 (Thick) sometime during flare a3 - In attenuator state 3 (Both) sometime during flare An - Attenuator state (0=None, 1=Thin, 2=Thick, 3=Both) at peak of flare DF - Front segment counts were decimated sometime during flare DR - Rear segment counts were decimated sometime during flare ED - Spacecraft eclipse (night) sometime during flare EE - Flare ended in spacecraft eclipse (night) ES - Flare started in spacecraft eclipse (night) FE - Flare ongoing at end of file FR - In Fast Rate Mode FS - Flare ongoing at start of file GD - Data gap during flare GE - Flare ended in data gap GS - Flare started in data gap MR - Spacecraft in high-latitude zone during flare NS - Non-solar event PE - Particle event: Particles are present PS - Possible Solar Flare; in front detectors, but no position Pn - Position Quality: P0 = Position is NOT valid, P1 = Position is valid Qn - Data Quality: Q0 = Highest Quality, Q11 = Lowest Quality SD - Spacecraft was in SAA sometime during flare SE - Flare ended when spacecraft was in SAA SS - Flare started when spacecraft was in SAA Geostationary Operational Environmental Satellite Data: Date - The date when the flare occurred Start - Flare start time Peak - Flare peak time End - Flare end time Classification - Solar flares are classified as A, B, C, M or X according to the peak flux (in watts per square metre, W/m2) of 100 to 800 picometre X-rays near Earth, as measured on the GOES spacecraft. Within a class there is a linear scale from 1 to 9. B [deg] - Heliographic latitude B; positive: North, negative: South LCM [deg] - Longitudinal distance from the Sun's central meridian For presentation of solar flares in 1996-2006 we used SOHO/EIT images which recorded by the SOHO Extreme ultraviolet Imaging Telescope observing at wavelegths of 171, 195, 284 and 304 Angstrom. In a given interval usually the image taken at 195 Angstrom is used which are closest in time to the largest flare of that interval. For the years after 2010 the images recorded at wavelegths of 171 Angstrom by Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory(SDO) are used. Derived position data of flares in 2011-2014 were taken from the list of SolarSoft Latest Events at LMSAL based on SECCHI/EUVI (BEACON) or EIT High Cadence Wavelength or SDO/AIA Flare Locator Images. Some additional data and corrections were taken from the GOES XRAY event list available at http://hesperia.gsfc.nasa.gov/goes/goes_event_listings/.