Numerical simulation of circumcometary quasi-parallel shock waves

Details Numerical simulation of circumcometary quasi-parallel shock waves Numerical simulation of circumcometary quasi-parallel shock waves

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987kosis..25..952l&link_type=abstract

Kosmicheskie Issledovaniia (ISSN 0023-4206), vol. 25, Nov.-Dec. 1987, p. 952-957. In Russian.

Astronomy and Astrophysics

Astronomy

Astronomical Models, Cometary Atmospheres, Plasma Interactions, Shock Waves, Solar Wind, Algorithms, Maxwell-Boltzmann Density Function

Scientific paper

Numerical simulation indicates that the diffuse structure of a circumcometary quasi-parallel shock wave (theta less than 45 deg) is due to the development of Alfven oscillations and the ejection of cometary ions into the unperturbed solar-wind stream. In the foreshock, a resonant Alfven mode develops along with a firehose instability with a wavelength of 0.9 Rci; in the transition region, perturbations arise which are connected with the development of a cyclotron instability with a wavelength of 3 Rci. Here, the isotropization of the velocity distribution function of cometary ions is shown to break down in the case of a significant acceleration of ions along the magnetic field. The characteristic shock-wave thickness amounts to 4-5 Rci.

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