Accession Number:

ADA295448

Title:

Solar Flare MHD.

Descriptive Note:

Final rept. 1 Jan 91-31 Dec 94,

Corporate Author:

NEW YORK UNIV NY MAGNETO-FLUID DYNAMICS DIV

Personal Author(s):

Report Date:

1994-12-31

Pagination or Media Count:

17.0

Abstract:

Our research program dealt with physics of the solar atmosphere, particularly solar flares and the problem of solar coronal heating. Our approach was both analytical and computational. 3D magnetic reconnection. We investigated both driven and spontaneous 3D line tied reconnection. We found fast timescales, compatible with flare data, and markable similarity between drive reconnection, caused by footpoint motion, and spontaneous reconnection, caused by a newly discovered coalescene instability. Boundary conditions for the solar corona. We derived improved boundary conditions using analytic solutions of the wave propagation problem in a stratified medium. Ballooning modes. We studied ballooning modes in classical fluids and the effects of boundary conditions and rotation on plasma pressure driven ballooning modes. We found a new two dimensional prominence model, and analyzed its ballooning stability. Numerical Tools. We developed new numerical tools for solving the MHD equations. We produced a fast, robust, and highly accurate finite difference code, CHTH. We also be an developing an adaptive, unstructured mesh, finite element MHD code. AN

Subject Categories:

  • Astrophysics
  • Plasma Physics and Magnetohydrodynamics

Distribution Statement:

APPROVED FOR PUBLIC RELEASE