Relativistic simulations of rotational core collapse - II. Collapse dynamics and gravitational radiation

By H. Dimmelmeier, J. Font, E. Mueller. 2002

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We have performed hydrodynamic simulations of relativistic rotational supernova core collapse in axisymmetry and have computed the gravitational radiation emitted by such an event. The Einstein equations are formulated using the confor- mally flat metric approximation, and the corresponding hydrodynamic equations are written as a first-order flux-conservative hyperbolic system. Details of the methodology and of the numerical code have been given in an accompanying paper. We have simulated the evolution of 26 models in both Newtonian and relativistic gravity. The initial configurations are dierentially rotat- ing relativistic 4=3-polytropes in equilibrium which have a central density of 10 10 gc m 3 . Collapse is initiated by decreasing the adiabatic index to some prescribed fixed value. The equation of state consists of a polytropic and a thermal part for a more realis- tic treatment of shock waves. Any microphysics like electron capture and neutrino transport is neglected. Our simulations show that the three dierent types of rotational supernova core collapse and gravitational waveforms identified in previous Newtonian simulations (regular collapse, multiple bounce collapse, and rapid collapse) are also present in relativistic gravity. However, ro- tational core collapse with multiple bounces is only possible in a much narrower parameter range in relativistic gravity. The relativistic models cover almost the same range of gravitational wave amplitudes (4 10 21 h TT 3 10 20 for a source at a distance of 10 kpc) and frequencies (60 Hz 1000 Hz) as the corresponding Newtonian ones. Averaged over all models, the total energy radiated in the form of gravitational waves is 8:2 10 8 Mc 2 in the relativistic case, and 3:6 10 8 Mc 2 in the Newtonian case. For all collapse models that are of the same type in both Newtonian and relativistic gravity, the gravitational wave signal is of lower amplitude. If the collapse type changes, either weaker or stronger signals are found in the relativistic case. For a given model, relativistic gravity can cause a large increase of the characteristic signal frequency of up to a factor of five, which may have important consequences for the signal detection. Our study implies that the prospects for detection of gravita- tional wave signals from axisymmetric supernova rotational core collapse do not improve when taking into account relativistic gravity. The gravitational wave signals obtained in our study are within the sensitivity range of the first generation laser interfer- ometer detectors if the source is located within the Local Group. An online catalogue containing the gravitational wave signal amplitudes and spectra of all our models is available at the URL http://www.mpa-garching.mpg.de/Hydro/hydro.html.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3b04835b647dde73330f8dd4c282381cbaba31d3

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Citations in the corpus

Science case for the Einstein telescope (2019, background): “This phenomenon is central to most models today, with the exception of models of rare events involving significant rotation, which may be powered magneto-hydrodynamically and where the dynamics proceeds on shorter timescales [117–126].”
The astrophysical gravitational wave stochastic background (2011, methodology): “…calculated the stochastic background that results from the birth of neutron stars at cosmological distances, using relativistic numerical models of core collapse (Dimmelmeier et al. 2002), and updating the previous study by Coward et al. (2001), based on newtonian models (Zwerger & Mueller 1997).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, methodology): “We have implemented our relativistic ray-by-ray-plus method using the framework of two existing codes, the time-explicit relativistic hydrodynamics code CoCoNuT (Dimmelmeier et al. 2002a) and the implicit neutrino transport code VERTEX (Rampp & Janka 2002; Buras et al. 2006b).”
The basics of gravitational wave theory (2005, background): “Even without the growth of instabilities, the asymmetric dynamics of core collapse is likely to lead to wave emission which would be detectable within the Local Group of galaxies, with perhaps an event every few years detectable by advanced interferometers [73].”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “ng co re, which produces a time-dependent quadrupole (or higher) GW emission. Following the ﬁrst stud y by Mu¨ller, most studies of the past thirty have focused on the so-called bounce signals (e.g., [98, 99, 100, 101, 102, 103, 104, 105, 106, 107, 108, 109, 110, 111, 112]) and references therein). ”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS (2012, methodology): “We analyze the GW emission for several 2D simulations performed with the general relativistic neutrino hydrodynamics code Vertex-CoCoNuT (Müller et al. 2010) or its (pseudo)-Newtonian counterpart Vertex-Prometheus (Rampp & Janka 2002; Buras et al. 2006).”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “ how the assumption of uniform rotation aects the universality by considering dierentially rotating stars. Dierential rotation is important in proto-neutron stars formed after supernova explosions [177,178], whose dierential rotation may last for ˘1 minute, and in hypermassive neutron stars formed a”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “Most early investigations were limited to the collapse and bounce of rapidly rotating iron cores (Müller 1982; Mönchmeyer et al. 1991; Yamada & Sato 1995; Zwerger & Müller 1997; Dimmelmeier et al. 2002; Kotake et al. 2003; Ott et al. 2004).”
Physics, Astrophysics and Cosmology with Gravitational Waves (2009, background): “While supernova simulations generally suggest that the amplitude of emitted gravitational waves is small [147], numerical simulations of the aftermath of neutron-star coalescence suggest the possibility of very powerful gravitational-wave emission [60].”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “…understanding of the GW signal from a CCSN is for the most part derived from the analysis of 2D (axisymmetric) simulations (Finn & Evans 1990; Dimmelmeier et al. 2002, 2007; Shibata & Sekiguchi 2004; Kotake et al. 2009; Marek et al. 2009; Murphy et al. 2009; Cerdá-Durán et al. 2013; Mueller…”
Toward Gravitational Wave Signals from Realistic Core-Collapse Supernova Models (2003, background): “This is a relatively small rotation rate compared with those typically assumed in parameter studies based on rotating polytropes (see, e.g., Zwerger & Müller 1997; Dimmelmeier et al. 2002; Ott et al. 2004).”