Nonlocal thermal transport in solar flares

Details Nonlocal thermal transport in solar flares Nonlocal thermal transport in solar flares

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..904k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 15, 1987, p. 904-912. NASA-Navy-supported research.

Astronomy and Astrophysics

Astrophysics

30

Solar Atmosphere, Solar Flares, Solar Temperature, Atmospheric Models, Chromosphere, Heat Transfer, Magnetohydrodynamics, Temperature Profiles

Scientific paper

A flaring solar atmosphere is modeled assuming classical thermal transport, locally limited thermal transport, and nonlocal thermal transport. The classical, local, and nonlocal expressions for the heat flux yield significantly different temperature, density, and velocity profiles throughout the rise phase of the flare. Evaporation of chromospheric material begins earlier in the nonlocal case than in the classical or local calculations, but reaches much lower upward velocities. Much higher coronal temperatures are achieved in the nonlocal calculations owing to the combined effects of delocalization and flux limiting. The peak velocity and momentum are roughly the same in all three cases. A more impulsive energy release influences the evolution of the nonlocal model more than the classical and locally limited cases.

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