2003
DOI: 10.1103/physrevlett.91.201102
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Consequences of Nuclear Electron Capture in Core Collapse Supernovae

Abstract: The most important weak nuclear interaction to the dynamics of stellar core collapse is electron capture, primarily on nuclei with masses larger than 60. In prior simulations of core collapse, electron capture on these nuclei has been treated in a highly parameterized fashion, if not ignored. With realistic treatment of electron capture on heavy nuclei come significant changes in the hydrodynamics of core collapse and bounce. We discuss these as well as the ramifications for the post-bounce evolution in core c… Show more

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Cited by 251 publications
(359 citation statements)
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“…The range of T considered varies from T 9 = 1 up to T 9 = 10, in T 9 (GK) units, whereas the range in ρY e varies from ρY e = 10 6 mol/cm 3 up to ρY e = 10 10 mol/cm 3 . This grid of ρY e and T includes those ranges relevant for astrophysical scenarios related to the silicon-burning stage in a presupernova star [3] (ρY e = 10 7 mol/cm 3 and T 9 = 3), as well as scenarios related to precollapse of the core [44] and thermonuclear runaway type-Ia supernova [45] (ρY e = 10 9 mol/cm 3 and T 9 = 10).…”
Section: B Stellar Weak-decay Ratesmentioning
confidence: 99%
“…The range of T considered varies from T 9 = 1 up to T 9 = 10, in T 9 (GK) units, whereas the range in ρY e varies from ρY e = 10 6 mol/cm 3 up to ρY e = 10 10 mol/cm 3 . This grid of ρY e and T includes those ranges relevant for astrophysical scenarios related to the silicon-burning stage in a presupernova star [3] (ρY e = 10 7 mol/cm 3 and T 9 = 3), as well as scenarios related to precollapse of the core [44] and thermonuclear runaway type-Ia supernova [45] (ρY e = 10 9 mol/cm 3 and T 9 = 10).…”
Section: B Stellar Weak-decay Ratesmentioning
confidence: 99%
“…Nevertheless, the two spin cases we consider here in the elastic coherent scattering limit will serve as a guide to the behavior of the nuclear cross sections in general and, in particular, encompass the case of free nucleons. Typical mean nuclear masses in the density regime where SUSY interactions could play a significant role are A ≈ 100 to 200, though the actual NSE distribution of nuclear abundances is sensitive to entropy, neutron excess, the history of electron capture reactions and neutrino transport [24,25].…”
Section: Nuclear Physicsmentioning
confidence: 99%
“…In type II supernovae, they are among the nuclei that dominate the change in electronto-baryon ratio in the pre-supernova stage and thereby affect the structure of the star prior to the collapse [11][12][13]. In the Chandrasekhar-mass model for type Ia supernovae, ECs on iron-group nuclei take place in the wake of the thermonuclear flame, which leads to a reduction of the pressure and a retardation of the expansion of the star [14].…”
mentioning
confidence: 99%