Ramachandran, Babulakshmanan and Smith, Michael D. (2006) The influence of the Mach number on the stability of radiative shocks. Monthly Notices of the Royal Astronomical Society, 366 (2). pp. 586-608. ISSN 0035-8711. (The full text of this publication is not available from this repository)
We study the stability properties of hydrodynamic shocks with finite Mach numbers. The linear analysis supplements previous analyses which took the strong shock limit. We derive the linearized equations for a general specific heat ratio as well as temperature and density power-law cooling functions, corresponding to a range of conditions relevant to interstellar atomic and molecular cooling processes. Boundary conditions corresponding to a return to the upstream temperature (R= 1) and to a cold wall (R= 0) are investigated. We find that for Mach number M > 5, the strong shock overstability limits are not significantly modified. For M < 3, however, shocks are considerably more stable for most cases. In general, as the shock weakens, the critical values of the temperature power-law index (below which shocks are overstable) are reduced for the overtones more than for the fundamental, which signifies a change in basic behaviour. In the R= 0 scenario, however, we find that the overstability regime and growth rate of the fundamental mode are increased when cooling is under local thermodynamic equilibrium. We provide a possible explanation for the results in terms of a stabilizing influence provided downstream but a destabilizing effect associated with the shock front. We conclude that the regime of overstability for interstellar atomic shocks is well represented by the strong shock limit unless the upstream gas is hot. Although molecular shocks can be overstable to overtones, the magnetic field provides a significant stabilizing influence.
|Divisions:||Faculties > Science Technology and Medical Studies > School of Physical Sciences|
|Depositing User:||Michael Smith|
|Date Deposited:||08 Sep 2008 23:13|
|Last Modified:||09 Jun 2014 09:26|
|Resource URI:||http://kar.kent.ac.uk/id/eprint/8320 (The current URI for this page, for reference purposes)|