X-ray bright point flares due to magnetic reconnection |
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| Authors: | L Van Driel-Gesztelyi B Schmieder G Cauzzi N Mein A Hofmann N Nitta H Kurokawa P Mein J Staiger |
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| Institution: | (1) Observatoire de Paris, Section de Meudon, DASOP, F-92195 Meudon, Principal Cedex, France;(2) Kiso Observatory, The University of Tokyo, Mitake, Kiso, 397-01 Nagano, Japan;(3) Observatoire de Paris, Section de Meudon, DASOP, F-92195 Meudon, Principal Cedex, France;(4) Institute for Astronomy, University of Hawaii, 96822 Honolulu, HI, U.S.A.;(5) Observatoire de Paris, Section de Meudon, DASOP, F-92195 Meudon, Principal Cedex, France;(6) Astrophysikaliches Institut Potsdam, Sonnenobservatorium Einsteinturm, D-14473 Potsdam, Germany;(7) Lockheed Palo Alto Research Laboratory, B/252, 0/91-30, 3251 Hanover Street, 94304 Palo Alto, CA, U.S.A.;(8) Applied Research Corporation, 20785 Landover, MD, U.S.A.;(9) Kwasan and Hida Observatories, Kyoto University, Kamitakara, 506-13 Gifu, Japan;(10) Observatoire de Paris, Section de Meudon, DASOP, F-92195 Principal Cedex, France;(11) Kiepenheuer-Institut für Sonnenphysik, D-79104 Freiburg, Germany |
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| Abstract: | Ground-based optical observations coordinated with Yohkoh/SXT X-ray observations of an old, disintegrating bipolar active region AR NOAA 7493 (May 1, 1993) provided a multiwavelength data base to study a flaring  active region X-ray bright point (XBP) of about 16 hr lifetime, and the activity related to it in different layers of the solar atmosphere. The XBP appeared to be related to a new minor bipole of about 1020 Mx. Superposed on a global evolution of soft X-ray brightness, the XBP displayed changes of brightness, lasting for 1–10 min. During the brightenings the XBP apparently had a spatial structure, which was (tiny) loop-like rather than point-like. The X-ray brightenings were correlated with chromospheric activity: (i) brightenings of underlying chromospheric faculae, and (ii) appearance of strong turbulent velocities in the arch filament system. We propose that the XBP brightenings were due to reconnection of the magnetic field lines (sketched in 3D) between the new bipole and a pre-existing plage field induced by the motion of one of the new pores (v = 0.2 km s–1) towards the plage, and that the XBP itself was a reconnected hot loop between them. |
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