Dynamics of radiative supernova remnants

Details Dynamics of radiative supernova remnants Dynamics of radiative supernova remnants

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...334..252c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 1, 1988, p. 252-265.

Computer Science

Sound

244

Astronomical Models, Gas Dynamics, Stellar Evolution, Supernova Remnants, Equations Of Motion, Radiative Transfer, Shock Wave Propagation

Scientific paper

The authors study the evolution of a supernova remnant (SNR) evolving in a homogeneous, uniform medium. They have concentrated on the transition from the adiabatic stage to the radiative pressure-driven snowplow stage, and the possible further establishment of a momentum-conserving snowplow stage. In the numerically simulated example (ejecta mass of 3 M_sun;, ambient hydrogen density of 0.1 cm-3), the radiative stage begins after less than one sound crossing time from the end of the free-expansion stage, and as a result the interior of the blast wave never completely settles to the Sedov-Taylor similarity solution. The authors also provide a simple physical model for the overall dynamics and present analytic approximations, good to a few percent in radius and velocity when compared with the numerical simulations.

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