Supernova Nucleosynthesis in Massive Stars
نویسندگان
چکیده
منابع مشابه
Nucleosynthesis in massive stars revisited
We have performed the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in a finely-zoned stellar model computed from the onset of central hydrogen burning through explosion as a Type II supernova. Calculations were done for 15 M⊙, 20 M⊙, and 25 M⊙ Pop I stars using the most recently available set of experimental and theoretical nuclear data, revi...
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We investigate hydrodynamical and nucleosynthetic properties of the jet-induced explosion of a population III 40M⊙ star and compare the abundance patterns of the yields with those of the metal-poor stars. We conclude that (1) the ejection of Fe-peak products and the fallback of unprocessed materials can account for the abundance patterns of the extremely metal-poor (EMP) stars and that (2) the ...
متن کاملNuclear Aspects of Nucleosynthesis in Massive Stars
Nuclear reactions play a major role not only in the nucleosynthetic processes determining the elemental abundances in the solar system and the Galaxy but also for determining structure and final fate of a star. Massive stars (> 8M⊙) experience a number of burning phases before they explode as type II supernovae after the collapse of the Fe core. Important nuclear reactions in the late burning s...
متن کاملModeling The Nucleosynthesis Of Massive Stars
This overview discusses issues relevant to modeling nucleosynthesis in type II supernovae and implications of detailed studies of the ejecta. After a brief presentation of the most common approaches to stellar evolution and parameterized explosions, the relevance of a number of nuclei to obtain information on the evolution and explosion mechanisms is discussed. The paper is concluded by an outl...
متن کاملLedoux-convection in protoneutron stars – a clue to supernova nucleosynthesis
Two-dimensional (2D) hydrodynamical simulations of the deleptonization of a newly formed neutron star (NS) were performed. Driven by negative lepton fraction and entropy gradients, convection starts near the neutrinosphere about 20– 30 ms after core bounce, but moves deeper into the protoneutron star (PNS), and after about one second the whole PNS is convective. The deleptonization of the star ...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1996
ISSN: 0252-9211
DOI: 10.1017/s0252921100008022