Volume 478, Number 1, January IV 2008
|Page(s)||17 - 29|
|Published online||12 November 2007|
Supernova remnant evolution in uniform and non-uniform media
Unit for Space Physics, School of Physics, North-West University, 2520 Potchefstroom, South Africa e-mail: Stefan.Ferreira@nwu.ac.za
2 Centre for High Performance Computing (CHPC), CSIR Campus, 15 Lower Hope St. Rosebank, Cape Town, South Africa
Accepted: 25 October 2007
Aims.In this work numerical simulations showing the time evolution of supernova remnants (SNRs) in uniform and non-uniform interstellar medium (ISM) are presented.
Methods.We use a hydrodynamic model including a kinematic calculation of the interstellar magnetic field. Important parameters influencing SNR evolution include the ejecta mass and energy of the remnant, as well as the ISM density and adiabatic index.
Results.By varying these parameters we constructed an analytical expression giving the return time of the SNR reverse shock to the origin, in terms of these parameters. We also found that the reverse shock spends half of its time moving outward and the other half returning to the origin. Also computed is SNR evolution in non-uniform media where the blast wave moves from one medium into either a less or more dense medium. As the SNR moves into a medium of higher density a reflection wave is created at the interface between the two media which is driven back toward the center. This drives mass via a nonspherical flow away from the discontinuity. As this wave moves inward it also drags some of the ISM field lines (if the field is parallel with the interface) with it and heats the inside of the SNR resulting in larger temperatures in this region. When a SNR explodes in a medium with a high density and the blast wave propagates into a medium with a lower density, a cavity is being blown away changing the geometry of the high density region. Also, once the forward shock moves into the medium of less density a second reverse shock will start to evolve in this region.
Key words: stars: supernovae: general / ISM: supernovae remnants / methods: numerical, magnetohydrodynamics (MHD) / shock waves / ISM: cosmic rays
© ESO, 2008
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