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Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation
The major uncertainties involved in the Chandrasekhar mass models for Type Ia supernovae (SNe Ia) are related to the companion star of their accreting white dwarf progenitor (which determines theExpand
Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution
Abstract We present new nucleosynthesis yields as functions of the stellar mass, metallicity, and explosion energy (corresponding to normal supernovae and hypernovae). We apply the results to theExpand
Galactic Chemical Evolution: Carbon through Zinc
We calculate the evolution of heavy-element abundances from C to Zn in the solar neighborhood, adopting our new nucleosynthesis yields. Our yields are calculated for wide ranges of metallicity (Z =Expand
An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295
The prompt γ-ray emission from γ-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation,Expand
Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + NE + MG cores.
Helium cores in stars with masses near 10 M/sub sun/ are evolved from the helium burning phase; the outer edge of the core is fitted to the boundary conditions at the bottom of the hydrogen-richExpand
Nucleosynthetic signatures of the first stars
TLDR
The discovery of HE1327–2326 is reported, a subgiant or main-sequence star with an iron abundance about a factor of two lower than that of HE0107–5240, suggesting a similar origin of the abundance patterns. Expand
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies
After the Big Bang, production of heavy elements in the early Universe takes place starting from the formation of the first stars, their evolution, and explosion. The first supernova explosions haveExpand
Accreting white dwarf models for type I supernovae. I. Presupernova evolution and triggering mechanisms
The evolution of carbon-oxygen white dwarfs accreting helium in binary systems has been investigated from the onset of accretion up to the point at which a thermonuclear explosion occurs as aExpand
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