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Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions
Nucleosynthesis, light curves, explosion energies, and remnant masses are calculated for a grid of supernovae resulting from massive stars with solar metallicity and masses from 9.0 to 120 solarExpand
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Formation of Double Neutron Star Systems
Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergersExpand
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Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos
One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so-called p-process nuclei from A = 92 to 126. Both the lighter and heavier p-process nuclei are adequatelyExpand
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Nucleosynthesis in the hot convective bubble in core-collapse supernovae
As an explosion develops in the collapsed core of a massive star, neutrino emission drives convection in a hot bubble of radiation, nucleons, and pairs just outside a proto-neutron star. ShortlyExpand
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Equation-of-state dependence of the gravitational-wave signal from the ring-down phase of neutron-star mergers
Neutron-star (NS) merger simulations are conducted for 38 representative microphysical descriptions of high-density matter in order to explore the equation-of-state dependence of the postmergerExpand
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Axisymmetric general relativistic simulations of the accretion-induced collapse of white dwarfs
The accretion-induced collapse (AIC) of a white dwarf may lead to the formation of a protoneutron star and a collapse-driven supernova explosion. This process represents a path alternative toExpand
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Neutrino signatures of supernova forward and reverse shock propagation
A few seconds after bounce in a core-collapse supernova, the shock wave passes the density region corresponding to resonant neutrino oscillations with the 'atmospheric' neutrino mass difference. TheExpand
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Neutrino-driven supernovae: An accretion instability in a nuclear physics controlled environment
New simulations demonstrate that low-mode, nonradial hydrodynamic instabilities of the accretion shock help starting hot-bubble convection in supernovae and thus support explosions by theExpand
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Neutrino emission from type II supernovae: an analysis of the spectra
Une methode de Monte Carlo est utilisee pour calculer le spectre des neutrinos de tous types, pour 2 stades differents apres l'effondrement du noyau de fer d'une etoile de 20 M ○. . Les resultatsExpand
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