The Solar Minimum Active Region 7978, Its X2.6/1B Flare,CME, and Interplanetary Shock Propagation of 9 July 1996 |
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| Authors: | Dryer M Andrews M D Aurass H DeForest C Galvin A B Garcia H Ipavich F M Karlický M Kiplinger A Klassen A Meisner R Paswaters S E Smith Z Tappin S J Thompson B J Watari S I Michels D J Brueckner G E Howard R A Koomen M J Lamy P Mann G Arzner K Schwenn R |
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| Institution: | (1) NOAA Space Environment Center, Boulder, CO, 80303, U.S.A.;(2) Hughes STX/NRL, Washington, D.C, 20375, U.S.A.;(3) Astrophysikalisches Institut Potsdam, D-14472, Germany;(4) Stanford University, NASA Goddard SFC, Greenbelt, MD, 20771, U.S.A.;(5) University of Colorado, Boulder, CO, 80309, U.S.A.;(6) Naval Research Laboratory, Washington, D. C., 20375, U.S.A.;(7) University of Birmingham, Birmingham, B15 275, U.K.;(8) Space Applications Corp., NASA Goddard SFC, Greenbelt, MD, 20771, U.S.A.;(9) Communications Research Laboratory, Koganei, Tokyo, 184, Japan;(10) Laboratoire Astronomie Spatiale, 13376 Marseille Cedex 12, France;(11) Max-Planck Institut für Aeronomie, D-37189 Katlenburg-Lindau, Germany;(12) University of Maryland, College Park, MD, 20742, U.S.A.;(13) Astronomical Institute, Ond ejov Observatory, 25165, Czech Republic;(14) Institut für Angewandte Physik der Universität Bern, CH-3012 Bern, Switzerland;(15) University of Colorado, Denver, CO, 80201;(16) SFA, Inc., Landover, MO, 20785 |
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| Abstract: | The first X-class flare in four years occurred on 9 July 1996. This X2.6/1B flare reached its maximum at 09:11 UT and was located in active region 7978 (S10° W30°) which was an old-cycle sunspot polarity group. We report the SOHO LASCO/EIT/MDI and SOONSPOT observations before and after this event together with Yohkoh SXT images of the flare, radio observations of the type II shock, and GOES disk-integrated soft X-ray flux during an extended period that included energy build-up in this active region.The LASCO coronagraphs measured a significant coronal mass ejection (CME) on the solar west limb beginning on 8 July at about 09:53 UT. The GOES 8 soft X-ray flux (0.1–0.8 nm) had started to increase on the previous day from below the A-level background (10-8 W m-2). At the start time of the CME, it was at the mid-B level and continued to climb. This CME is similar to many events which have been seen by LASCO and which are being interpreted as disruption of existing streamers by emerging flux ropes.LASCO and EIT were not collecting data at the time of the X-flare due to a temporary software outage. A larger CME was in progress when the first LASCO images were taken after the flare. Since the first image of the 'big' CME was obtained after the flare's start time, we cannot clearly demonstrate the physical connection of the CME to the flare. However, the LASCO CME data are consistent with an association of the flare and the CME. No eruptive filaments were observed during this event.We used the flare evidence noted above to employ in real time a simplified Shock-Time-of-Arrival (STOA) algorithm to estimate the arrival of a weak shock at the WIND spacecraft. We compare this prediction with the plasma and IMF data from WIND and plasma data from the SOHO/CELIAS instrument and suggest that the flare - and possibly the interplanetary consequences of the 'big' CME - was the progenitor of the mild, high-latitude, geomagnetic storm (daily sum of Kp=16+, Ap=8) on 12 July 1996. We speculate that the shock was attenuated enroute to Earth as a result of interaction with the heliospheric current/plasma sheet.presently at High Altitude Observatory, Boulder, CO80309, U.S.A.presently at Naval Research Laboratory, Washington DC, 20375, U.S.A. |
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