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- W2063804558 abstract "The strong degeneracy of the 12C ignition layer on an accreting neutron star results in a hydrodynamic thermonuclear runaway, in which the nuclear heating time becomes shorter than the local dynamical time. We model the resulting combustion wave during these superbursts as an upward-propagating detonation. We solve the reactive fluid flow and show that the detonation propagates through the deepest layers of fuel and drives a shock wave that steepens as it travels upward into lower density material. The shock is sufficiently strong on reaching the freshly accreted H/He layer that it triggers unstable 4He burning if the superburst occurs during the latter half of the regular type I bursting cycle; this is likely the origin of the bright type I precursor bursts observed at the onset of superbursts. The cooling of the outermost shock-heated layers produces a bright, ≈0.1 s, flash that precedes the type I burst by a few seconds; this may be the origin of the spike seen at the burst onset in 4U 1820-30 and 4U 1636-54, the only two bursts observed with RXTE at high time resolution. The dominant products of the 12C detonation are 28Si, 32S, and 36Ar. Gupta et al. showed that a crust composed of such intermediate-mass elements has a larger heat flux than one composed of iron-peak elements and helps bring the superburst ignition depth into better agreement with values inferred from observations." @default.
- W2063804558 created "2016-06-24" @default.
- W2063804558 creator A5063290216 @default.
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- W2063804558 date "2007-12-01" @default.
- W2063804558 modified "2023-10-03" @default.
- W2063804558 title "Carbon Detonation and Shock‐Triggered Helium Burning in Neutron Star Superbursts" @default.
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- W2063804558 doi "https://doi.org/10.1086/522111" @default.
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