3-D MHD simulations of the effect of comoving discontinuities in the solar wind on cometary plasma tails

Details 3-D MHD simulations of the effect of comoving discontinuities in the solar wind on cometary plasma tails 3-D MHD simulations of the effect of comoving discontinuities in the solar wind on cometary plasma tails

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...295..529r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 295, no. 2, p. 529-550

Astronomy and Astrophysics

Astrophysics

20

Astronomical Models, Comet Tails, Comets, Discontinuity, Interplanetary Medium, Magnetohydrodynamics, Solar Wind, Space Plasmas, Three Dimensional Models, Computerized Simulation, Interplanetary Magnetic Fields, Solar Magnetic Field

Scientific paper

The effects of several types of tangential discontinuities in the solar wind on cometary plasma tails are studied using a time-dependent 3-D MHD model (Schmidt-Voigt 1989). First, a change in the solar wind direction by 6 deg has been simulated. This model shows a gradual turn of the plasma tail towards the new flow direction. A rotation of the interplanetary magnetic field (IMF) by 90 deg leads to the formation of a pair of symmetric tail rays folding towards the main tail when the tail is viewed along the new IMF. When viewed along the original IMF a narrowing of the tail, starting at the nucleus, can be observed. A combination of both parameter changes results in the formation of a one-sided ray and a turn of the main tail towards the ray. Comparison with ground-based observations show, for all three simulation runs, agreement with some of the characteristic features seen in cometary ion tails.

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