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One-armed Spiral Instability in a Low- <i>T</i> /| <i>W</i> | Postbounce Supernova Core

Christian D. OttMax-Planck-Institut für Gravitationsphysik, Albert-Einstein-Institut, Am Mühlenberg 1, D-14476 Golm, GermanyShangli OuCenter for Computation and Technology, Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803Joel E. TohlineCenter for Computation and Technology, Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803Adam BurrowsSteward Observatory and Department of Astronomy, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721

2005en

ABI

Annotatsiya

A three-dimensional, Newtonian hydrodynamic technique is used to follow the postbounce phase of a stellar core collapse event. For realistic initial data we have employed post core-bounce snapshots of the iron core of a 20 solar mass star. The models exhibit strong differential rotation but have centrally condensed density stratifications. We demonstrate for the first time that such postbounce cores are subject to a so-called low-T/|W| nonaxisymmetric instability and, in particular, can become dynamically unstable to an m=1 - dominated spiral mode at T/|W| ~ 0.08. We calculate the gravitational wave emission by the instability and find that the emitted waves may be detectable by current and future GW observatories from anywhere in the Milky Way.

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DOI: 10.1086/431305

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