Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..418d&link_type=abstract
The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand
Astronomy and Astrophysics
Astronomy
Scientific paper
Mass loss from massive stars (⪆ 8 M&sun;) can result in the formation of circumstellar wind blown cavities surrounding the star, bordered by a thin, dense, cold shell. When the star explodes as a core-collapse supernova (SN), the resulting shock wave will interact with this modified medium around the star, rather than the interstellar medium. We explore the formation of these bubbles around various types of stars, and the evolution of SNe within these wind-blown bubbles. The evolution depends primarily on a single parameter Λ, the ratio of the mass of the dense shell to that of the ejected material. We investigate the evolution for different values of this parameter. We also plot approximate X-ray surface brightness plots from the simulations. For very small values Λ ≪ 1 the effect of the shell is negligible as expected. Values of Λ ⪉ 1 affect the SN evolution, but the SN 'forgets' about the existence of the shell in about 10 doubling times or so. The X-ray luminosity increases by a couple of orders of magnitude upon shock-shell collision. The remnant density profile changes after the shock-shell impact, and consequently the X-ray emission from the remnant will also change. X-ray images will show the presence of a double-shelled structure as the reflected shock begins to move inwards. The density discontinuity behind the inward-moving shock wave is found to be Rayleigh-Taylor unstable. Larger values of Λ result in more SN energy being expended to the shell. The resulting reflected shock moves quickly back to the origin, and consequently the ejecta are thermalized rapidly. The evolution of the remnant is speeded up, and the entire remnant appears bright in X-rays. If Λ ≫ 1 then a substantial amount of energy may be expended in the shell. In the extreme case the SN may go directly from the free-expansion to the adiabatic stage, bypassing the Sedov stage.
No associations
LandOfFree
SN Evolution in the Environment of Massive Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with SN Evolution in the Environment of Massive Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and SN Evolution in the Environment of Massive Stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1301867