Hideyuki Umeda

Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation

We calculate explosive nucleosynthesis in Chandrasekhar mass models for Type Ia Supernovae(SNe Ia) to obtain new constraints on the rate of matter accretion onto the progenitor white dwarf and on the ignition density of central carbon deflagration. The calculated abundance of the Fe-group neutron-rich nuclei is highly sensitive to the electron captures taking place in the central layers. The yields obtained from a slow central deflagration, and from a fast deflagration or delayed detonation in the outer layers, are combined and put to comparison with solar isotopic abundances. We found that (1) to avoid too large ratios of

An Unusual Supernova in the Error Box of the Gamma-Ray Burst of 25 April 1998

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A 'hypernova' model for the supernova associated with the gamma-ray burst of 25 April 1998

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Galactic Chemical Evolution: Carbon through Zinc

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NUCLEOSYNTHESIS OF ZINC AND IRON PEAK ELEMENTS IN POPULATION III TYPE II SUPERNOVAE: COMPARISON WITH ABUNDANCES OF VERY METAL POOR HALO STARS

Fe and

Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution

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Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae

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First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

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One Hundred First Stars : Protostellar Evolution and the Final Masses

Fe, the ignition density should be as low as \ltsim 2 \e9 \gmc, and that (2) to avoid the overproduction of

Variations in the Abundance Pattern of Extremely Metal-Poor Stars and Nucleosynthesis in Population III Supernovae

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