Nucleosynthesis in Supernovae
نویسندگان
چکیده
منابع مشابه
Nucleosynthesis in Core Collapse Supernovae
We present the basic properties of the yields of our latest set of presupernova evolution and explosive nucleosynthesis of massive stars in the range between 11 and 120 M having solar and zero metallicity.
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Core collapse supernovae are the leading actor in the story of the cosmic origin of the chemical elements. Existing models, which generally assume spherical symmetry and parameterize the explosion, have been able to broadly replicate the observed elemental pattern. However, inclusion of neutrino interactions produces noticeable improvement in the composition of the ejecta when compared to obser...
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Presupernova evolution and explosive nucleosynthesis in massive stars for main-sequence masses from 13 M ⊙ to 70 M ⊙ are calculated. We examine the dependence of the super-nova yields on the stellar mass, 12 C(α, γ) 16 O rate, and explosion energy. The supernova yields integrated over the initial mass function are compared with the solar abundances.
متن کاملNucleosynthesis in Type Ia Supernovae
Among the major uncertainties involved in the Chandrasekhar mass models for Type Ia supernovae are the companion star of the accreting white dwarf (or the accretion rate that determines the carbon ignition density) and the flame speed after ignition. We present nucleosynthesis results from relatively slow deflagration (1.5 3 % of the sound speed) to constrain the rate of accretion from the comp...
متن کاملNeutron-rich Nucleosynthesis in Carbon Deflagration Supernovae
Accreting carbon-oxygen white dwarfs approaching the Chandrasekhar mass may provide a substantial fraction of Type Ia supernovae. The hydrodynamics of nuclear burning in these models remains uncertain, but all current models are characterized by an initial period of slow, nearly laminar Ñame propagation at a well-known conductive speed. For cold white dwarfs and slow accretion, the density at t...
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ژورنال
عنوان ژورنال: Physical Review Letters
سال: 1999
ISSN: 0031-9007,1079-7114
DOI: 10.1103/physrevlett.82.5198