Selfinhibiting heat flux
Abstract
Heat transfer through weakly magnetized diffuse astrophysical plasmas excites whistlers. This leads to electron whistler resonant scattering, a reduction of the electron mean free path, and heat flux inhibition. However, only whistlers propagating at a finite angle to the magnetic field (offaxis) can scatter the heat flux carrying electrons. Thus the level of heat flux inhibition along the magnetic field lines depends on the presence of offaxis whistlers. We obtain a solution of the Boltzmann equation with the whistler wave equation and show that if epsilonthbetae>>10^4, where epsilon^th is the thermal collisional Knudsen number and beta_e is the ratio of the electron pressure to the magnetic energy density, then scattering of heat flux carrying electrons by offaxis whistlers, which are shown to propagate at about 65delta, is efficient enough to lead to heat flux inhibition along field lines. The inhibition so obtained is proportional to (epsilon^thbeta_e)^1.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 November 1998
 DOI:
 10.1046/j.13658711.1998.01770.x
 arXiv:
 arXiv:astroph/9807025
 Bibcode:
 1998MNRAS.301...49P
 Keywords:

 CONDUCTION;
 HYDRODYNAMICS;
 MAGNETIC FIELDS;
 PLASMAS;
 WAVES;
 Astrophysics
 EPrint:
 doi:10.1046/j.13658711.1998.01770.x