Numerical modeling of interaction between solar wind and cometary plasma

Details Numerical modeling of interaction between solar wind and cometary plasma Numerical modeling of interaction between solar wind and cometary plasma

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986rpspr...1..100l&link_type=abstract

In its USSR Report: Space (JPRS-USP-86-0010 p 100 (SEE N86-20178 10-88) Transl. into ENGLISH from Kosmicheskiye Issledovaniya

Astronomy and Astrophysics

Astronomy

Astronomical Models, Cometary Atmospheres, Plasma Interactions, Solar Wind, Collisionless Plasmas, Cometary Magnetospheres, Heavy Ions, Larmor Radius, Planetary Magnetic Fields, Plasma Temperature, Shock Waves

Scientific paper

The collisionless particle-in-cell technique is used to study the interaction of the solar wind with heavy cometary ions and the related magnetic-field dynamics. An analysis is made of the parameters of the solar-wind stagnation zone. The structure of the external shock wave and transition region, and the configuration of the induced magnetosphere. It is concluded that the passage of a solar-wind stream through a near-cometary region produces an entrainment of the ionized component of the comet, leading to the formation of a stream of the ionized component of the comet, leading to the formation of a stream of cometary ions with a characteristic temperature that is significantly greater than the temperature transverse to the magnetic field as well as the proton stagnation temperature. The comet is specifically characterized by the presence of energetic ions at the shock front. Therefore the thickness of the shock front and the structure of the transition region have a characteristic scale that is determined by the Larmor radius of the heavy ion.

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