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The Interaction of the Solar Wind with a Comet

Conference paper

Abstract

In 1951 Biermann [2] detected the solar wind as the agent, which shapes the cometary plasma to an extended tail. Numerical model calculations for the interaction of the solar wind with a comet started in 1967 with a simplified one-dimensional model [3]. Since then the model prospered and matured from hydrodynamics to MHD and grew from one to three dimensions [5]. A comprehensive presentation of the results was given by Schmidt and Wegmann [6]. Recently the model got new impact from the collaboration with the group of Huebner in Los Alamos [4]. Last year it had to face the major challenge posed by the ICE spacecraft, which made the first in situ measurements of a cometary plasma. I report here on some improvements which we included recently in this “Schmidt-Wegmann-model”. Furthermore I present some results, which we obtain for a comet like comet Giacobini-Zinner and compare these with the data from the ICE spacecraft.

Keywords

Solar Wind Field Line Shock Front Interplanetary Magnetic Field Elastic Collision 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

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Copyright information

© Springer-Verlag Berlin Heidelberg 1987

Authors and Affiliations

  1. 1.Institut für AstrophysikMax-Planck-Institut für Physik und AstrophysikGarchingFed. Rep. of Germany

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