Propagation of two-fluid interplanetary shock waves

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Abstract

A two-fluid time-dependent analytical model of the perturbed solar wind is presented. The expansion of newly emitted material, caused, for instance, by the outburst of a solar flare, is simulated by a spherical piston. The electron collision time is phenomenologically decreased to account for a transit from a collisional (near the Sun) to a collisionless regime (at 1 AU). This effectively inhibits thermal conductivity and enhances ion-electron heat exchange. For a given thermal conductivity in the limit of strong coupling, one-fluid flow in a thermally conducting medium is recovered. A pattern of flow which resembles one-fluid flow in an adiabatic medium may be obtained if heat is removed from the perturbed plasma into the propelling plasma.
Original languageEnglish
Pages (from-to)5897 - 906
JournalJournal of Geophysical Research C: Oceans
Volume84
Issue numberA10
StatePublished - 1979

Keywords

  • interplanetary matter
  • shock waves
  • solar wind
  • wave propagation

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