Statistics – Computation
Scientific paper
May 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...215..347c&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 215, no. 2, May 1989, p. 347-359. Research supported by MPI.
Statistics
Computation
24
B Stars, Computational Astrophysics, O Stars, Stellar Winds, Supernova Remnants, Astronomical Models, Stellar Temperature, Wave Propagation
Scientific paper
Supernova ejecta created by the explosion of an O-B star are expected to expand through a pre-existing bubble generated by the previous fast stellar wind. In order to study the interaction between such a bubble and the supernova remnant with an appreciable spatial resolution, two separate numerical computations were performed making use of moving grids. First, the bubble evolution was simulated until the steady state was reached. Then, the supernova remnant expansion was simulated in such a way as to obtain the Chevalier (1975, 1976) solution as long as the remnant itself travels through the unperturbed wind. Finally, the remnant merged in the bubble, whose presence was recognized through the boundary conditions at the outer side of the remnant grid. It turns out that the geometry of ring-like supernova remnants such as the Cygnus Loop can be readily understood. For closer comparisons with observational data, however, the red giant phase of the progenitor must be considered. During this stage, the gas of the bubble moves inward while a rarefaction wave travels through the bubble cooling it.
Ciotti Luca
D'Ercole Annibale
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