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How Massive Single Stars End Their Life
How massive stars die—what sort of explosion and remnant each produces—depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are theExpand
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Nucleosynthesis in massive stars with improved nuclear and stellar physics
We present the first calculations to follow the evolution of all stable nuclei and their radioactive progeni- tors in stellar models computed from the onset of central hydrogen burning throughExpand
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Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure
The evolution of rotating stars with zero-age main-sequence (ZAMS) masses in the range 8-25 M☉ is followed through all stages of stable evolution. The initial angular momentum is chosen such that theExpand
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THE EFFECTS OF BINARY EVOLUTION ON THE DYNAMICS OF CORE COLLAPSE AND NEUTRON STAR KICKS
We systematically examine how the presence in a binary affects the final core structure of a massive star and its consequences for the subsequent supernova explosion. Interactions with a companionExpand
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The supernova channel of super-AGB stars
We study the late evolution of solar metallicity stars in the transition region between white dwarf formation and core collapse. This includes the super-asymptotic giant branch (super-AGB, SAGB)Expand
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Presupernova Evolution of Rotating Massive Stars. II. Evolution of the Surface Properties
We investigate the evolution of the surface properties of models for rotating massive stars, i.e., their luminosities, effective temperatures, surface rotational velocities, and surface abundances ofExpand
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A simple approach to the supernova progenitor–explosion connection
We present a new approach to understand the landscape of supernova explosion energies, ejected nickel masses, and neutron star birth masses. In contrast to other recent parametric approaches, ourExpand
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Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties
We study the impact of large-scale perturbations from convective shell burning on the core-collapse supernova explosion mechanism using three-dimensional (3D) multi-group neutrino hydrodynamicsExpand
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On the Stability of Very Massive Primordial Stars
The stability of metal-free very massive stars (Z \ 0; M \ 120¨500 is analyzed and compared M _ ) with metal-enriched stars. Such zero-metallicity stars are unstable to nuclear-powered radialExpand
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MULTI-INSTRUMENT X-RAY OBSERVATIONS OF THERMONUCLEAR BURSTS WITH SHORT RECURRENCE TIMES
Type I X-ray bursts from low-mass X-ray binaries result from a thermonuclear runaway in the material accreted onto the neutron star. Although typical recurrence times are a few hours, consistent withExpand
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