Coronal proton transport in the presence of Alfven waves and implications for gamma-ray burst models

Details Coronal proton transport in the presence of Alfven waves and implications for gamma-ray burst models Coronal proton transport in the presence of Alfven waves and implications for gamma-ray burst models

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...373..289s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 373, May 20, 1991, p. 289-293.

Other

4

Gamma Ray Bursts, Magnetohydrodynamic Waves, Solar Corona, Solar Corpuscular Radiation, Solar Protons, Coronal Loops, Solar Flares, Solar Magnetic Field, Wave Excitation, Wave Propagation

Scientific paper

The transport of fast (above 10 MeV) protons in the corona is considered when their density and anisotropy are sufficiently large to excite Alfven waves. It is shown that, for coronal propagation lengths of 3 x 10 to the 8th cm or 5 x 10 to the 8th cm, Alfven waves scatter the protons and make them almost isotropic. The Alfven wave instability remains in a marginally stable state in which the proton anisotropy is just large enough to excite Alfven waves to a level which would eliminate any greater ansiotropy. As a result, the proton path lengths are 6-65 times larger than in the absence of Alfven waves and their mean free paths are 3 x 10 to the 6th-4x 10 to the 7th cm (i.e., the protons are well contained). For proton coronal propagation lengths of 3 x 10 to the 8th or 5 x 10 to the 8th cm, loop densities of at least 4 x 10 to the 10th cm are required for a magnetic field of 100 G for the June 7, 1980 flare. In general, only loops of high density and/or low magnetic field are consistent with the other observations of this flare. This theory is compared with the theory of Bespalov et al. (1987).

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