A 2-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. 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 adiabatic medium may be recovered if heat is removed from the perturbed plasma into the propelling plasma. The perturbed flow consists of a thermal precursor which is followed by a shock across which electrons are isothermal while protons are compressed and heated. Finally, we show that the post-shock rise and fall of density cannot be used to distinguish piston-driven waves from blast waves.
|Title of host publication||Solar and Interplanetary Dynamics|
|Editors||M. Dryer, E. Tandberg-Hanssen|
|Place of Publication||Dordrecht|
|Number of pages||5|
|ISBN (Print)||978-90-277-1162-5, 978-90-277-1163-2|
|State||Published - 1980|
|Name||International Astronomical Union Symposia|