Abstract
This paper presents models of optical emission line features that characterise catastrophic cooling in radiative shocks. The computations are based on a 1-D magnetohydrodynamic model. Runaway cooling results in the formation of secondary shocks which travel through the previously shocked cooling layer. Several filaments of emission with specific properties and spectral signatures are produced.
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References
Dopita M.A.: 1977,Astrophys. J. Suppl.,33, 437.
Gaetz T.J., Edgar J. & Chevalier R.A.:1988,Astrophys. J.,329, 927.
Innes D.E.: 1988, In: Kundt W. (ed) Supernova Shells and their Birth Events, p74.
Innes D.E.:1992,Astron. & Astrophys.,256, 660.
Innes D.E., Giddings J.R. & Falle S.A.E.G.:1987a,Mon. Not. R. astr. Soc.,226, 67.
Innes D.E., Giddings J.R. & Falle S.A.E.G.:1987b,Mon. Not. R. astr. Soc.,227, 1021.
Raymond J.C.: 1979,Astrophys. J. Suppl.,39, 1.
Shull J.M. & McKee C.F.: 1979,Astrophys. J.,227, 131.
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Innes, D.E. Catastrophic cooling diagnostics. Astrophys Space Sci 216, 311–316 (1994). https://doi.org/10.1007/BF00982510
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DOI: https://doi.org/10.1007/BF00982510