Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..565..222b&link_type=abstract
YOUNG SUPERNOVA REMNANTS: Eleventh Astrophysics Conference. AIP Conference Proceedings, Volume 565, pp. 222-225 (2001).
Astronomy and Astrophysics
Astrophysics
Supernova Remnants, Supernovae
Scientific paper
An important ingredient in hydrodynamical models of SNR evolution is the incorporation of radiative cooling. Unfortunately, the cooling of hot (T=104-108 K) plasmas depends sensitively upon the ionization state of the individual ions. This frequently departs from collisional ionization equilibrium. As a result, calculating an accurate cooling generally requires the solution of over a hundred differential equations. This computational requirement is generally prohibitive for three dimensional simulations. We discuss here progress on the development of a simple 2-dimensional solution for the cooling coefficient due to elements heavier than H and He. The cooling depends only on electron temperature and the mean charge of the ion population. In the test cases we consider, it provides a good approximation to the non-equilibrium cooling coefficient in cases for which the cooling due to these trace elements exceeds 10% of that due to H and He. .
Benjamin Robert A.
Benson Bradford Adam
Cox Donald P.
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