Franziska Brachwitz

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

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

^{54}

Nuclear cross sections, nuclear structure and stellar nucleosynthesis☆

Cr/

Element synthesis in stars

^{56}

Nucleosynthesis and stellar evolution

Fe and

Nucleosynthesis in SNe Ia as a function of the burning front propagation

^{50}

Yields from Type Ia Supernovae

Ti/

The physics of type Ia supernovae

^{56}

Nuclear physics : a key ingredient in astrophysical modeling

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

Supernova Nucleosynthesis and Galactic Evolution

^{58}