Friedrich-Karl Thielemann

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

Probing the gravitational well: No supernova explosion in spherical symmetry with general relativistic Boltzmann neutrino transport

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Simulation of the Spherically Symmetric Stellar Core Collapse, Bounce, and Postbounce Evolution of a Star of 13 Solar Masses with Boltzmann Neutrino Transport, and Its Implications for the Supernova Mechanism

Cr/

Computational methods for nucleosynthesis and nuclear energy generation

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Conservative general relativistic radiation hydrodynamics in spherical symmetry and comoving coordinates

Fe and

Silicon Burning. II. Quasi-Equilibrium and Explosive Burning

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An Adaptive Grid, Implicit Code for Spherically Symmetric, General Relativistic Hydrodynamics in Comoving Coordinates

Ti/

Explosive Nucleosynthesis in Type I and Type II Supernovae

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Synthesis of Heavy Elements in the Ejecta of Neutron Star Mergers

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

Astrophysical Implications of the QCD phase transition

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