Nonlocal Heat Transport in the Solar Wind

Details Nonlocal Heat Transport in the Solar Wind Nonlocal Heat Transport in the Solar Wind

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...462.1005c&link_type=abstract

Astrophysical Journal v.462, p.1005

Astronomy and Astrophysics

Astronomy

10

Sun: Solar Wind, Sun: Corona

Scientific paper

It is shown that a nonlocal, suprathermal tail originated near the solar corona base dominates the conductive energy flux at distances r ≥ 2 Rsun. A nonlocal analytical expression for the electron heat flux in weakly collisional plasmas is derived by solving the Fokker-Planck equation in a narrow, tail energy range. A correction to the anisotropy of the distribution function due to the divergent magnetic field lines was included. This term is essential to recover from the delocalization prescription, in the limit r ≥ 6Rsun, the well-known Hollweg's Ansatz for the "collisionless" heat flux. In the intermediate region 2 Rsun ≤ r ≤ 6 Rsun, the nonlocal convolution smoothly interpolates between the classical Spitzer-Härm's formula and the so-called collisionless régime.

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