Thermal instability of a radiative and resistive coronal plasma

Details Thermal instability of a radiative and resistive coronal plasma Thermal instability of a radiative and resistive coronal plasma

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...333..953s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 333, Oct. 15, 1988, p. 953-964. NASA-NSF-supported research.

Physics

9

Magnetohydrodynamic Stability, Plasma Radiation, Radiative Transfer, Solar Corona, Thermal Instability, Astronomical Models, Solar Magnetic Field, Solar Prominences

Scientific paper

Thermal instability is believed to determine the evolution and formation of cool structures in the solar atmosphere such as the transition region and prominences (or filaments). The linear modes that arise in a sheared, force-free, magnetic field due to thermal instability are studied numerically. Previous studies have considered separately modes that arise due to the effects of radiation, compression, anisotropic thermal conduction, and ohmic heating. Here the results of such studies are integrated, first by presenting simple arguments that illustrate the essential physics of ideal, sheared-field, condensation modes, and second by showing numerically how finite resistivity affects the condensational instability in parameter regimes applicable to the solar corona.

Affiliated with

Also associated with

No associations

Rating

Thermal instability of a radiative and resistive coronal plasma does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Thermal instability of a radiative and resistive coronal plasma, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Thermal instability of a radiative and resistive coronal plasma will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1598219