Numerical MHD Simulations of Post-Flare Loop Formation on the Sun: Allowing for Thermal-Conductivity Anisotropy

Details Numerical MHD Simulations of Post-Flare Loop Formation on the Sun: Allowing for Thermal-Conductivity Anisotropy Numerical MHD Simulations of Post-Flare Loop Formation on the Sun: Allowing for Thermal-Conductivity Anisotropy

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46...67p&link_type=abstract

Astronomy Reports, Volume 46, Issue 1, January 2002, pp.67-73

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The process of post-flare loop formation, including the heating of flux tubes by hot chromospheric sources and their filling with plasma, is demonstrated by simulations in an MHD approximation. The loop is additionally heated at its apex by the interaction of oppositely directed plasma streams. Local coronal heating over the loop is also possible due to magnetic-field-line reconnection. A new version of the PERESVET code that can take into account anisotropy of the thermal conductivity of a plasma in a magnetic field was used for the computations.

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