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Contribution Details
| Type | Journal Article |
| Scope | Discipline-based scholarship |
| Title | Gravitational waves from supernova matter |
| Organization Unit |
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| Authors |
|
| Item Subtype | Original Work |
| Refereed | Yes |
| Status | Published in final form |
| Language |
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| Journal Title | Classical and Quantum Gravity |
| Geographical Reach | international |
| ISSN | 0264-9381 (P) 1361-6382 (E) |
| Volume | 27 |
| Number | 11 |
| Page Range | 114101 - 114111 |
| Date | 2010 |
| Abstract Text | We have performed a set of 11 three-dimensional magnetohydrodynamical (MHD) core-collapse supernova simulations in order to investigate the dependences of the gravitational wave signal on the progenitor's initial conditions. We study the effects of the initial central angular velocity and different variants of neutrino transport. Our models are started up from a 15Modot progenitor and incorporate an effective general relativistic gravitational potential and a finite temperature nuclear equation of state. Furthermore, the electron flavour neutrino transport is tracked by efficient algorithms for the radiative transfer of massless fermions. We find that non- and slowly rotating models show gravitational wave emission due to prompt- and lepton driven convection that reveals details about the hydrodynamical state of the fluid inside the protoneutron stars. Furthermore we show that protoneutron stars can become dynamically unstable to rotational instabilities at T/|W| values as low as ~2% at core bounce. We point out that the inclusion of deleptonization during the postbounce phase is very important for the quantitative gravitational wave (GW) prediction, as it enhances the absolute values of the gravitational wave trains up to a factor of ten with respect to a lepton-conserving treatment. |
| Digital Object Identifier | 10.1088/0264-9381/27/11/114101 |
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