Presupernova Structure of Massive Stars

Abstract

Issues concerning the structure and evolution of core collapse progenitor stars are discussed with an emphasis on interior evolution. We describe a program designed to investigate the transport and mixing processes associated with stellar turbulence, arguably the greatest source of uncertainty in progenitor structure, besides mass loss, at the time of core collapse. An effort to use precision observations of stellar parameters to constrain theoretical modeling is also described.

Proceedings for invited talk at High Energy Density Laboratory Astrophysics conference, Caltech, March 2010. Special issue of Astrophysics and Space Science, submitted for peer review: 7 pages, 3 figures

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Cited by in corpus (9)

• The Compactness of Presupernova Stellar Cores
• Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M${}_{\odot }$ Stars
• Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism
• A New Multi-Energy Neutrino Radiation-Hydrodynamics Code in Full General Relativity and Its Application to Gravitational Collapse of Massive Stars
• Pre-Supernova Outbursts via Wave Heating in Massive Stars II: Hydrogen-poor Stars
• Two-Dimensional Core-Collapse Supernova Models with Multi-Dimensional Transport
• A Diversity of Wave-driven Pre-supernova Outbursts
• The red supergiant and supernova rate problems: implications for core-collapse supernova physics
• Constraints on explosive silicon burning in core-collapse supernovae from measured Ni/Fe ratios