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- W2022279921 abstract "During a supernova explosion, a radiation-dominated shock (RDS) travels through its progenitor. A collisionless shock (CS) is usually assumed to replace it during shock breakout (SB). We demonstrate here that for some realistic progenitors enshrouded in optically thick winds, such as possibly SN 2008D, a CS forms deep inside the wind, soon after the RDS leaves the core, and therefore significantly before SB. The RDS does not survive the transition from the core to the thick wind when the wind close to the core is not sufficiently dense to compensate for the r−2 dilution of photons due to shock curvature. This typically happens when the shock velocity is |${lesssim } 0.1 {rm c} , (frac{u_{rm w}}{10,{rm km,s^{-1}}}) (frac{skew4 dot{M} }{5 times 10^{-4} , {rm M}_{odot }, {rm ,yr^{-1}}})^{-1} (frac{r_ast }{10^{13},{rm cm}})$|, where uw, |$skew4 dot{M} $| and r* are, respectively, the wind velocity, mass-loss rate and radius of the progenitor star. The radiative CS results in a hard spectrum of the photon flash at breakout, which would produce an X-ray flash. Cosmic ray acceleration would start before SB, for such progenitors. A fraction of secondary TeV neutrinos can reach the observer up to more than 10 h before the first photons from breakout, providing information on the invisible layers of the progenitor." @default.
- W2022279921 created "2016-06-24" @default.
- W2022279921 creator A5068633840 @default.
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- W2022279921 date "2015-04-10" @default.
- W2022279921 modified "2023-10-14" @default.
- W2022279921 title "Collisionless shocks and TeV neutrinos before Supernova shock breakout from an optically thick wind" @default.
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- W2022279921 doi "https://doi.org/10.1093/mnras/stv561" @default.
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