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High-beta Disruption in the Solar Atmosphere View all abstracts by submitter

Kiyoto Shibasaki   Submitted: 2001-05-10 11:48

The outer layers of X-ray loops in solar flares are known to be more active: they are hotter than the lower loops and above-the-loop-top hard X-ray sources are formed there. These phenomena are interpreted as the result of the reconnection above the loop, which convert magnetic energy into thermal and non-thermal energy of plasma. However, little direct evidence for the reconnection has been presented so far. This paper interprets the activity in the outer layer of flaring loops on a different scenario. Coronal loops filled with hot and dense plasma (high beta) or with fast plasma flow, surrounded by the low-beta corona, are unstable at their outer boundary where the curvature is convex outward and the density gradient is inward. The centrifugal force acting upward on the plasma in the loop can exceed that of gravity. This condition is favorable for localized interchange instability called "ballooning instability" and the plasma in the loop is ejected when the instability has developed into non-linear phase ("high-beta disruption"). This is a natural consequence of the high-beta (and/or the high velocity) plasma confined in a curved coronal loop. The high-beta disruption has many elements common to solar flares. In this paper, importance of the high-beta plasma is stressed, which is a neglected part of the solar activity so far.

Authors: Kiyoto Shibasaki
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Publication Status: ApJ (in press)
Last Modified: 2001-05-10 11:48
Go to main E-Print page  Gamma-Ray Line Observations of the 2000 July 14 Flare and SEP Impact on the Earth  Drifting radio bursts and fine structures in the 0.8-7.6 GHz frequency range observed in the NOAA 9077 AR (July 10-14, 2000) solar flares  Edit Entry  Download Preprint  Delete Entry 

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