On the Hot Gas Fraction in Supernova Remnants

Details On the Hot Gas Fraction in Supernova Remnants On the Hot Gas Fraction in Supernova Remnants

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...453..264h&link_type=abstract

Astrophysical Journal v.453, p.264

Astronomy and Astrophysics

Astronomy

4

Hydrodynamics, Ism: Bubbles, Ism: Supernova Remnants

Scientific paper

A grid of spherically symmetric numerical models of the evolution of supernova remnants is calculated, covering the ambient density range n0 = 0.001-100 hydrogen atoms cm-3 and with metallicities ranging from solar to primordial. These models are analyzed with the purpose of determining the relative mass fraction ɛhot of hot gas (T < 105 K) in the remnants as a function of time. From the work of Cioffi, McKee, and Bertschinger, we derive an analytical formula for ɛhot for times larger than the cooling time of the swept-up gas shell, and we demonstrate that all our model results are well fitted by this expression.
Such an analytic expression is useful in models of a multiphase interstellar medium, feedback mechanisms from supernovae in star-forming regions, and in models of galaxy formation and evolution in general.

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