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We compare calculations of r-process abundances with recent astronomical observations from extremely metal-deficient, neutron-capture-rich halo stars. We derive criteria to determine Th and U chronometric ages, and deduce astrophysical conditions under which the observed abundance patterns can be obtained under r-like conditions.
Recent progress in modeling type Ia supernovae by means of 3-dimensional hydrodynamic simulations as well as several of the still open questions are addressed in this review. It will be shown that the new models have considerable predictive power which allows us to study observable properties such as light curves and spectra without adjustable non-physical parameters. Finally, first results obtained...
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