Koichi Iwamoto

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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Radiation Hydrodynamics of SN 1987A. I. Global Analysis of the Light Curve for the First 4 Months

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THE TYPE IC HYPERNOVA SN 2002AP

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THE PECULIAR TYPE Ic SUPERNOVA 1997ef: ANOTHER HYPERNOVA

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Light Curve and Spectral Models for the Hypernova SN 1998bw Associated with GRB 980425

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The Role of Electron Captures in Chandrasekhar-Mass Models for Type Ia Supernovae

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Type Ia Supernovae: Their Origin and Possible Applications in Cosmology

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

Can Differences in the Nickel Abundance in Chandrasekhar-Mass Models Explain the Relation between the Brightness and Decline Rate of Normal Type Ia Supernovae?

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