Observations of The Magnetic Reconnection Signature of An M2 Flare on 2000 March 23

Details Observations of The Magnetic Reconnection Signature of An M2 Flare on 2000 March 23 Observations of The Magnetic Reconnection Signature of An M2 Flare on 2000 March 23

2009-07-27

arxiv.org/abs/0907.4541v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

19 pages, 6 figures, accepted by ApJ

Scientific paper

Multi-wavelength observations of an M 2.0 flare event on 2000 March 23 in NOAA active region 8910 provide us a good chance to study the detailed structure and dynamics of the magnetic reconnection region. In the process of the flare, extreme ultraviolet (EUV) loops displayed two times of sideward motions upon a loop-top hard X-ray source with average velocities of 75 and 25.6 km/s, respectively. We consider these two motions to be the observational evidence of reconnection inflow, and find an X-shaped structure upon the post-flare loops during the period of the second motion. Two separations of the flare ribbons are associated with these two sideward motions, with average velocities of 3.3 and 1.3 km/s, separately. Using the observation of photospheric magnetic field, the velocities of the sideward motions and the separations, we deduce the corresponding coronal magnetic field strength to be about 13.2-15.2 G, and estimate the reconnection rates to be 0.05 and 0.02 for these two magnetic reconnection processes, respectively. We also observe motions of bright points upward and downward along the EUV loops with velocities ranging from 45.4 to 556.7 km/s. A cloud of bright material flowing outward from the loop-top hard X-ray source with an average velocity of 51 km/s in the process of the flare may be accelerated by the tension force of the newly reconnected magnetic field lines. All the observations can be explained by schematic diagrams of magnetic reconnection.

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