Clear Evidence of Reconnection Inflow of a Solar Flare

Details Clear Evidence of Reconnection Inflow of a Solar Flare Clear Evidence of Reconnection Inflow of a Solar Flare

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...546l..69y&link_type=abstract

The Astrophysical Journal, Volume 546, Issue 1, pp. L69-L72.

Astronomy and Astrophysics

Astronomy

130

Magnetohydrodynamics: Mhd, Plasmas, Sun: Flares

Scientific paper

We found an important piece of evidence for magnetic reconnection inflow in a flare on 1999 March 18. The flare occurred on the northeast limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration events. The EUV observation of the same flare shows us a bubble-like void ejection. The core of this EUV void corresponds to the soft X-ray plasmoid. Moreover, as this void is ejected, magnetic reconnection occurs at the disconnecting point. A clear ongoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km s-1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA=0.001-0.03, where MA is an Alfvén Mach number of the inflow.

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