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Gravitational
Radiation from General Relativistic Rotational Core
Collapse with Microphysics (Extended Model Set) 

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H. Dimmelmeier (Section of Astrophysics, Astronomy & Mechanics, Aristotle University of Thessaloniki, Greece) C.D. Ott (Department of Astronomy and Steward Observatory, University of Arizona, U.S.A.) A. Marek H.T. Janka Simulations: We have simulated a set of 136 rotational supernova core collapse models in axisymmetry. To simulate these models, we numerically solve the fully general relativistic hydrodynamic equations in a fluxconservative formulation [Banyuls, et al., 1997] on a grid using spherical coordinates. For an accurate resolution of shocks, we have implemented a modern highresolution shockcapturing scheme, which uses characteristic information of relativistic hydrodynamics [Font, 2000]. The exact metric in the ADM spacetime foliation is approximated by assuming conformal flatness for the threemetric, which significantly reduces the complexity of the hydrodynamic and metric equations. As initial configuration we choose the presupernova stellar models e15a, e15b, e20a, e20b, s11.2, s15, s20, or s40 [Woosley, et al., 2002]. The progenitor models e15a, e15b, e20a, and e20b have an angular momentum distribution from stellar evolution calculations, while on the s11.2, s15, s20, and s40 models we impose rotation [Komatsu, et al., 1989a, Komatsu, et al., 1989b] with different rates and profiles. During core collapse, we utilize a microphysical equations of state specifically designed for supernova core collapse, either the one by Shen et al. (Shen EoS) [Shen, et al., 1998] or the one by Lattimer and Swesty (LS EoS) [Lattimer and Swesty, 1998]. To approximate the effects of neutrinos in the infall phase, a very efficient parametric deleptonization scheme is used [Liebendörfer, 2005]. Again, as for previous models with a more restricted selection of free parameters, we find that the gravitational wave burst signal from core bounce is very uniform. We also observe the effects of the centrifugal barrier on the collapse dynamics for rapidly rotating models, which effectively prevents the collapsing core from reaching the very high rotation rates needed for becoming unstable to dynamical rotation instabilities. This mechanism also limits the amplitude of the waveform for gravitational radiation. A detailed description of the models and other interesting information can be found in a published article [Dimmelmeier, et al., 2008]. We provide a waveform catalog of all simulated models. Additionally, you can click on the following shortcuts to view figures of the waveforms in various formats or download raw data of the waveforms. Figures of the waveforms in EPS format Figures of the waveforms in JPG format
Gravitational wave signal data
Density evolution data
