Dynamics and spectra of magnetically cushioned radiative shocks

Details Dynamics and spectra of magnetically cushioned radiative shocks Dynamics and spectra of magnetically cushioned radiative shocks

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..660i&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 2, p. 660-672.

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Magnetic Field Configurations, Plasma Physics, Radiative Transfer, Shock Waves, Supernova Remnants, Astronomical Models, Astronomical Spectroscopy, Computational Astrophysics, Emission Spectra, Photoionization

Scientific paper

This paper investigates the effects of magnetic fields on the evolution and spectral appearance of unstable radiative shocks. In this work, a detailed treatment of the ionization evolution, the photoionizing radiation and its transfer through the gas, is coupled to a 1D MHD scheme. The cushioning effect of the magnetic field on the formation of secondary shocks in the postshock cooling flow is clearly demonstrated by our results. The field strengths required to suppress shock formation are at least a factor two greater than predicted by linear stability analysis. Thus a field strength, transverse to the flow, of 9 micro-G is required to suppress shock formation behind a 175 km/s shock, travelling into a density of 1/cu cm. Inclusion of the magnetic field results in realistic pressures and densities in the cool postshock photoionized shell. This allows us to follow the dynamics of the evolving photoionization zone where much of the low excitation optical radiation is emitted. We discuss characteristic features in the spectra of unstable shocks and describe spectral diagnostics, based on the optical and UV line ratios and spatial intensity distributions, for their identification.

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