Two-Fluid Motion of Plasma in Alfvén Waves and the Heating of Solar Coronal Loops

Details Two-Fluid Motion of Plasma in Alfvén Waves and the Heating of Solar Coronal Loops Two-Fluid Motion of Plasma in Alfvén Waves and the Heating of Solar Coronal Loops

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...511..958w&link_type=abstract

The Astrophysical Journal, Volume 511, Issue 2, pp. 958-964.

Astronomy and Astrophysics

Astronomy

25

Magnetohydrodynamics: Mhd, Plasmas, Sun: Corona, Sun: X-Rays, Gamma Rays, Waves

Scientific paper

Taking the effect of two-fluid motion of plasma in Alfvén waves into account, a nonzero parallel electric field can rise within the wave itself under collisionless conditions. This leads to a kinetic dissipation of Alfvén waves by the wave-particle resonant interaction and electron heating along the ambient magnetic field lines. Employing the drift kinetic equation, we investigated this electron-heating mechanism under the cool ion approximation. The result shows that the damping rate and the heating rate obviously depend on the strength distribution of the ambient magnetic field, and that they reach their maximum values at B_0=B_m and B_0=1+2alpha^1/2B_m, respectively, for the perturbed field of deltaB~B^alpha_0, where B_m is the ambient magnetic field strength when v_A=v_Te. Finally, we propose that this heating mechanism can be applied to explain the brightness distribution of solar soft X-ray coronal loops.

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