The eruption of supernova shock waves

Epstein, Richard I.

doi:10.1086/183486

Cited by 19 publications

(11 citation statements)

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“…The shock wave moving through the star is strongly radiation dominated, giving rise to a burst of radiation when the shock wave reaches an optical depth ∼ , where c is the speed of c/u light and u is the shock velocity. The radiation accelerates the gas ahead of the shock wave, so that the shock wave disappears; a gas-dominated shock wave then forms in the surrounding medium when the supernova radius has roughly doubled (Epstein 1981;Fransson 1982). This evolution is shown well in the simulation by Ensman (1994) which has parameters intended for SN 1987A.…”

Section: Early X-ray Emissionmentioning

confidence: 99%

Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D

Chevalier

Fransson

2008

ApJ

135

191

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The X-ray transient 080109, associated with SN 2008D, can be attributed to the shock breakout emission from a normal Type Ib/c supernova. If the observed emission is interpreted as thermal emission, the temperature and radiated energy are close to expectations, considering that scattering dominates absorption processes so that spectrum formation occurs deep within the photosphere. The X-ray emission observed at ∼10 days is attributed to inverse Compton scattering of photospheric photons with relativistic electrons produced in the interaction of the supernova with the progenitor wind. A simple model for the optical/ultraviolet emission from shock breakout is developed and applied to SN 1987A, SN 1999ex, SN 2008D, and SN 2006aj, all of which have optical emission observed at day. The emission from the first three can plausibly be attributed to shock breakout emission.The photospheric temperature is most sensitive to the radius of the progenitor star core and the radii in these cases are in line with expectations from stellar evolution. The early optical/ultraviolet observations of SN 2006aj cannot be accommodated by a nonrelativistic shock breakout model in a straightforward way.

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Section: Early X-ray Emissionmentioning

confidence: 99%

Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D

Chevalier

Fransson

2008

ApJ

135

191

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“…Klein & Chevalier (1978) found for normal Type II SNe that a considerable amount of energy is emitted in the keV range as a result of the formation of a viscous shock. However, the existence of this is controversial, and depends on the e ciency of preacceleration of the gas (Epstein 1981). If included, the X-ray emission should be added to the otherwise roughly blackbody-shaped burst spectrum.…”

Section: Modelmentioning

confidence: 99%

The Line Emission from the Circumstellar Gas around SN 1987A

Lundqvist¹,

Fransson²

1996

ApJ

134

164

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The narrow emission lines from the inner ring around SN 1987A during the rst 2000 days are modeled assuming that the ring was ionized by radiation accompanying the supernova breakout. The analysis extends that in Lundqvist & Fransson (1991) to include an improved description for the geometry, a multi-density structure of the emitting gas, results from improved calculations for the evolution of the EUV radiation from the outburst, and updated atomic data. To model the light curves of the lines, the ring has to be optically thick to the ionizing radiation, as is the case for a ring geometry, but not for a spherical shell. The density of the observed gas in the ring ranges from 1

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“…The non-thermal flash is detectable by current X-ray telescopes and may be detectable out to 10's of Mpc by km-scale neutrino telescopes. PACS numbers: 97.60.Bw,*43.25.Cb, *43.40.Jc, 95.30.Jx It has long been suggested that an intense burst of X-ray radiation is expected to be emitted at the initial phases of a SN explosion, once the radiation mediated blast wave reaches the edge of the star [1][2][3][4][5][6]. If the star is surrounded by a sufficiently optically thick shell of circum-stellar matter (CSM), e.g.…”

mentioning

confidence: 99%

X-rays, γ-rays and neutrinos from collisionless shocks in supernova wind breakouts

Katz¹,

Sapir²,

Waxman³

2011

Proc. IAU

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Abstract. Some of the observed bursts of X-rays/Gamma-rays associated with supernovae (SNe) as well as very luminous SNe may result from the breakout of the SN shock from an optically thick wind surrounding the progenitor. We show that in such scenarios a collisionless shock necessarily forms during the shock breakout. An intense non-thermal flash of 1 MeV gamma rays, hard X-rays and multi-TeV neutrinos is produced simultaneously with and following the typical soft X-ray breakout emission, carrying similar or larger energy than the soft emission. The non-thermal flash is detectable by current X-ray telescopes and may be detectable out to 10's of Mpc by km-scale neutrino telescopes.

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The eruption of supernova shock waves

Cited by 19 publications

References 0 publications

Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D

Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D

The Line Emission from the Circumstellar Gas around SN 1987A

X-rays, γ-rays and neutrinos from collisionless shocks in supernova wind breakouts

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