Journal Article

Multifluid numerical models of wind-swept clumps

A. J. Lim and A. C. Raga

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 303, issue 3, pages 546-554
Published in print March 1999 | ISSN: 0035-8711
Published online March 1999 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1046/j.1365-8711.1999.02253.x
Multifluid numerical models of wind-swept clumps

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Abstract

We present 2D axisymmetric numerical models of the dynamics of a multifluid interaction between a high-velocity rarefied wind of ionization fraction 0.5 and dense clumps of varying ionization fraction. The difference in the relative ram pressure acting on the neutral and ionic components of the clump results in a separation between the ionic and neutral bow shocks, which is an order of magnitude larger than that which would be expected from the different pressure to density ratios of the ions and neutrals. This results in the neutral bow shock leading for a low-ionization clump, and the ionic shock leading for a high-ionization clump. Simulated long-slit Hα spectra are calculated for each of three clump ionization fractions. For higher levels of clump ionization a narrow component at the preshock speed is clearly seen in the emission profile. Such a component is typically seen in spectroscopic observations of the Balmer filaments of supernova remnants.

Keywords: hydrodynamics; plasmas; supernova remnants

Journal Article.  3699 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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