Volume 401, Number 3, April III 2003
|Page(s)||1027 - 1038|
|Section||Interstellar and circumstellar matter|
|Published online||01 April 2003|
The evolution of mass loaded supernova remnants
II. Temperature dependent mass injection rates
Department of Physics & Astronomy, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
2 Instituto de Astronomia, UNAM, Campus Morelia, Apartado Postal 3-72, 58090 Morelia, Michoac an, Mexico
3 Department of Applied Mathematics, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
Corresponding author: J. M. Pittard, firstname.lastname@example.org
Accepted: 4 February 2003
We investigate the evolution of spherically symmetric supernova remnants in which mass loading takes place due to conductively driven evaporation of embedded clouds. Numerical simulations reveal significant differences between the evolution of conductively mass loaded and the ablatively mass loaded remnants studied in Paper I. A main difference is the way in which conductive mass loading is extinguished at fairly early times, once the interior temperature of the remnant falls below ~107 K. Thus, at late times remnants that ablatively mass load are dominated by loaded mass and thermal energy, while those that conductively mass load are dominated by swept-up mass and kinetic energy. Simple approximations to the remnant evolution, complementary to those in Paper I, are given.
Key words: ISM: kinematics and dynamics / ISM: supernova remnants / galaxies: ISM
© ESO, 2003
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