The Evolution of Supernovae in Circumstellar Wind-Blown Bubbles. I. Introduction and One-Dimensional Calculations

摘要: Mass loss from massive stars (8 M☉) can result in the formation of circumstellar wind-blown cavities surrounding star, bordered by a thin, dense, cold shell. When star explodes as core-collapse supernova (SN), resulting shock wave will interact with this modified medium around rather than interstellar medium. In work we first explore nature various evolutionary stages. This is followed study evolution SNe within these bubbles. The depends primarily on single parameter Λ, ratio mass dense shell to that ejected material. We investigate for different values parameter. also plot approximate X-ray surface brightness plots simulations. For very small Λ 1 effect negligible, one would expect. Values affect SN evolution, but "forgets" about existence 10 doubling times or so. remnant density profile changes, and consequently emission change. initial luminosity quite low, interaction increase 2-3 orders magnitude. As reflected begins move inward, images show presence double-shelled structure. Larger more energy being expended moves quickly back origin, ejecta are thermalized rapidly. speeded up, entire may appear bright X-rays. If 1, then substantial amount be extreme case go directly free expansion adiabatic stage, bypassing Sedov stage. Our results many cases SNR spends significant time bubble. low bubble delay onset stage end up reducing spent complicated makes it difficult infer mass-loss properties pre-SN studying SNR.