Tearing modes in solar coronal loops

Details Tearing modes in solar coronal loops Tearing modes in solar coronal loops

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348..778h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 348, Jan. 10, 1990, p. 778-780.

Astronomy and Astrophysics

Astrophysics

7

Coronal Loops, Magnetohydrodynamic Stability, Solar Corona, Tearing Modes (Plasmas), Magnetic Field Reconnection, Magnetohydrodynamic Waves, Solar Interior, Solar Magnetic Field

Scientific paper

It is shown that solar coronal-like magnetic loops, that is loops emerging from and reentering heavy plasma, are unstable to tearing modes. In particular, the previously made assumption of line tying to the heavy plasma, resulting in stabilization, is shown to be inapplicable because the growth rate is sub-Alfvenic in the entire loop, including the submerged part. In fact, it is shown that the tearing mode may grow faster than ordinarily surmised because the growth rate is determined by the average resistivity along an entire flux line rather than by the resistivity in the corona alone.

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