Axisymmetric General Relativistic Simulations of the Accretion-Induced Collapse of White Dwarfs

Details Axisymmetric General Relativistic Simulations of the Accretion-Induced Collapse of White Dwarfs Axisymmetric General Relativistic Simulations of the Accretion-Induced Collapse of White Dwarfs

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aps..aprb13006a&link_type=abstract

American Physical Society, APS April Meeting 2010, February 13-16, 2010, abstract #B13.006

Physics

Scientific paper

The accretion-induced collapse (AIC) of a white dwarf (WD) may lead to the formation of a protoneutron star and a collapse-driven supernova explosion. This process represents a path alternative to thermonuclear disruption of accreting white dwarfs in Type Ia supernovae. Motivated by the need for systematic predictions of the GW signature of AIC, we present results from an extensive set of general-relativistic AIC simulations using a microphysical finite-temperature equation of state and an approximate treatment of deleptonization during collapse. Investigating a set of 114 progenitor models in rotational equilibrium, with a wide range of rotational configurations, temperatures and central densities, we extend previous Newtonian studies and find that the GW signal has a generic shape akin to what is known as a ``Type III'' signal in the literature. We discuss the detectability of the emitted GWs. Some of our AIC models form massive quasi-Keplerian accretion disks after bounce. In rapidly differentially rotating models, the disk mass can be as large as ˜0.8-Msun. Slowly and/or uniformly rotating models produce much smaller disks. Finally, we find that the postbounce cores of rapidly spinning WDs can reach sufficiently rapid rotation to develop a nonaxisymmetric rotational instability. )

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