Gravitational Waves from Axisymmetric, Rotating Stellar Core Collapse

By Christian D. Ott, Adam Burrows, E. Livne, Rolf Walder. 2003

167 citations recorded by the source corpus.

We have carried out an extensive set of two-dimensional, axisymmetric, purely hydrodynamic calculations of rotational stellar core collapse with a realistic, finite-temperature nuclear equation of state and realistic massive star progenitor models. For each of the total number of 72 different simulations we performed, the gravitational wave signature was extracted via the quadrupole formula in the slow-motion, weak-field approximation. We investigate the consequences of variation in the initial ratio of rotational kinetic energy to gravitational potential energy and in the initial degree of differential rotation. Furthermore, we include in our model suite progenitors from recent evolutionary calculations that take into account the effects of rotation and magnetic torques. For each model, we calculate gravitational radiation waveforms, characteristic wave strain spectra, energy spectra, final rotational profiles, and total radiated energy. In addition, we compare our model signals with the anticipated sensitivities of the first- and second-generation LIGO detectors coming on line. We find that most of our models are detectable by LIGO from anywhere in the Milky Way.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f07ee3836121bdec61f555edfcf5b06d97b0a679

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

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).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “The computational grid employed here is set up to resemble a spherical-polar grid at radii greate than 20 km and gradually transitions to a Cartesian structure at smaller radii (Ott et al. 2004).”
The Spin Periods and Rotational Profiles of Neutron Stars at Birth (2005, methodology): “As with slowly rotating models, the greatest part of the gravitational wave emission will come from postbounce large-scale convective motions in the postshock region and in the PNS (Ott et al. 2004) and, possibly, from anisotropic neutrino emission (Burrows & Hayes 1996; Müller et al. 2004).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, background): “A version of this grid structure is plotted in Ott et al. (2004).”
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 NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, background): “…wide range of (sometimes extreme) astrophysical scenarios, such as rapidly rotating neutron stars (Cook et al. 1996), rigidly rotating disks (Kley & Schäfer 1999), and rotational core collapse (Shibata & Sekiguchi 2004; Cerdá-Durán et al. 2005; Ott et al. 2007a, 2007b; Dimmelmeier et al. 2007).”
Evolution and fate of very massive stars (2013, background): “…al. (2012, and references therein), the large angular momentum content is most interesting for the stars that just fall short of the minimum CO core mass for PCSN (since fast rotation plays an important role during the early collapse; Ott et al. 2004; O’Connor & Ott 2011; Chieffi & Limongi 2013).”
Effects of rotation on the evolution of primordial stars (2008, background): “Ott et al. (2004) show that rotation increases the amplitude of GW because of the induced anisotropy.”
Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation (2007, background): “Note that, due to the strong gravitational wave bursts that are signatures of the bounce of rapidly rotating cores, the associated supernovae may be centrally relevant to ongoing efforts to detect gravitational waves (Ott et al. 2004, 2007).”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, unknown): “…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 et al. 2013; Abdikamalov et al.…”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, result): “This is rather slow compared to the conditions considered in manyof the core-collapse simulations performed by other groups (e.g., Ott et al. 2004; Kotake et al. 2004).”
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). ”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “Thus they are good candidates for sizable gravitational-wave pulses from the moment of core bounce (e.g., Kotake et al. 2006; Ott et al. 2004).”