Journal ArticleDOI
On the problem of a shock wave arriving at the edge of a gas
TLDR
In this paper, the authors investigated what kind of phenomena may be expected when a shock wave propagates through a nonuniform medium of decreasing density and reaches the boundary where the density vanishes.Abstract:
An investigation was made as to what kind of phenomena may be expected when a shock wave propagates through a nonuniform medium of decreasing density and reaches the boundary where the density vanishes. This situation may arise for shock waves moving in plasmas sustained by magnetic pressure. (T.R.H.)read more
Citations
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Journal ArticleDOI
The expulsion of stellar envelopes in core-collapse supernovae
TL;DR: In this paper, the authors examined the relation between presupernova stellar structure and the distribution of ejecta in core-collapse supernovae of Types I, Ic, and II, under the approximations of adiabatic, spherically symmetric flow.
Journal ArticleDOI
Early Supernovae Light Curves Following the Shock Breakout
Ehud Nakar,Re'em Sari +1 more
Abstract: The first light from a supernova (SN) emerges once the SN shock breaks out of the stellar surface. The first light, typically a UV or X-ray flash, is followed by a broken power-law decay of the luminosity generated by radiation that leaks out of the expanding gas sphere. Motivated by recent detection of emission from very early stages of several SNe, we revisit the theory of shock breakout and the following emission, paying special attention to the photon-gas coupling and deviations from thermal equilibrium. We derive simple analytic light curves of SNe from various progenitors at early times. We find that for more compact progenitors, white dwarfs, Wolf-Rayet stars (WRs), and possibly more energetic blue-supergiant explosions, the observed radiation is out of thermal equilibrium at the breakout, during the planar phase (i.e., before the expanding gas doubles its radius), and during the early spherical phase. Therefore, during these phases we predict significantly higher temperatures than previous analysis that assumed equilibrium. When thermal equilibrium prevails, we find the location of the thermalization depth and its temporal evolution. Our results are useful for interpretation of early SN light curves. Some examples are (1) red supergiant SNe have an early bright peak in optical and UV flux, less than an hour after breakout. It is followed by a minimum at the end of the planar phase (about 10 hr), before it peaks again once the temperature drops to the observed frequency range. In contrast, WRs show only the latter peak in optical and UV. (2) Bright X-ray flares are expected from all core-collapse SNe types. (3) The light curve and spectrum of the initial breakout pulse hold information on the explosion geometry and progenitor wind opacity. Its spectrum in more compact progenitors shows a (nonthermal) power law and its light curve may reveal both the breakout diffusion time and the progenitor radius.
Journal ArticleDOI
The early uv/optical emission from core-collapse supernovae
Itay Rabinak,Eli Waxman +1 more
TL;DR: In this article, an approximate model of the early hours to days, UV/optical (UV/O) supernova emission is derived, which is produced by the expansion of the outer 10−2 M ☉ part of the shock-heated envelope, and precedes optical emission driven by radioactive decay.
Journal ArticleDOI
Supernova hosts for gamma-ray burst jets: dynamical constraints
TL;DR: In this article, the authors constrain a possible supernova origin for gamma-ray bursts (GRBs) by modelling the dynamical interaction between a relativistic jet and a stellar envelope surrounding it.
Journal ArticleDOI
Relativistic Shock Breakouts—A Variety of Gamma-Ray Flares: From Low-luminosity Gamma-Ray Bursts to Type Ia Supernovae
Ehud Nakar,Re'em Sari +1 more
TL;DR: In this article, the authors calculate the luminosity and spectrum produced by relativistic breakouts, and show that the resulting gamma-ray burst can be traced to the post-breakout acceleration of the gas during the planar phase.
References
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Journal ArticleDOI
On the propagation of shock waves through regions of non-uniform area or flow
TL;DR: In this paper, it is shown that the results of Moeckel and Chisnell's work can be obtained by the application of a simple rule, which must be satisfied by flow quantities along a characteristic to the flow quantities just behind the shock wave.
Journal ArticleDOI
Propagation of spherical shock waves in stars
TL;DR: In this article, the propagation of spherical shock waves through self-gravitating polytropic gas spheres such as stars, caused by an instantaneous central explosion of finite energy E, is discussed theoretically.
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