Magnetohydrodynamic (MHD) modelling of solar active phenomena via numerical methodsNumerical ideal MHD models for the study of solar active phenomena are summarized. Particular attention is given to the following physical phenomena: (1) local heating of a coronal loop in an isothermal and stratified atmosphere, and (2) the coronal dynamic responses due to magnetic field movement. The results suggest that local heating of a magnetic loop will lead to the enhancement of the density of the neighboring loops through MHD wave compression. It is noted that field lines can be pinched off and may form a self-contained magnetized plasma blob that may move outward into interplanetary space.
Document ID
19890023784
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Wu, S. T. (Alabama, University Huntsville, United States)
Date Acquired
August 13, 2013
Publication Date
January 1, 1988
Subject Category
Solar Physics
Meeting Information
Meeting: Southeastern Conference on Theoretical and Applied Mechanics