Reconnection in the Solar Corona: a study of the interaction of the 3-D Kelvin-Helmholtz instability and tearing instability

Details Reconnection in the Solar Corona: a study of the interaction of the 3-D Kelvin-Helmholtz instability and tearing instability Reconnection in the Solar Corona: a study of the interaction of the 3-D Kelvin-Helmholtz instability and tearing instability

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11c0723l&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11C-0723

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy

Scientific paper

For a typical configuration of magnetic field arcades in the Solar Corona, two instabilities are possible. First, in presence of velocity shear, which exists on the photospheric surface, the Kelvin-Helmholtz Instability (KHI) is excited. In 3-D, with differential rotation, The low speed shear KHI can drive magnetic reconnection [1]. The growth rate of the KHI is primarily controlled by the destabilizing effect of the velocity shear and by the stabilizing effect of a flow aligned magnetic field. However, the KHI is insensitive to the presence of resistivity. Second, the tearing instability can be considered a candidate for disrupting the equilibrium and for leading to Coronal Mass Ejections. Within a resistive MHD approach, the growth rate of the Tearing instability is negligible if the actual resistivity of the corona is used. Previous work [1] has suggested that when reconnection happens in presence of the KHI (in 3-D with differential rotation) the reconnection time scale is controlled by the KHI and not by the tearing instability. As a consequence, the reconnection rate becomes insensitive to resistivity and is primarily controlled by the velocity shear. In the present work, we explore the implications of the non-linear interaction of the 3-D KHI with differential rotation and reconnection for the Solar Corona. [1] J.U. Brackbill, D.A. Knoll, Phys Rev. Lett. 86, 2329, 2001

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