Gravitational wave burst signal from core collapse of rotating stars

By H. Dimmelmeier, Christian D. Ott, Andreas Marek, Hans-Thomas Janka. 2008

153 citations recorded by the source corpus.

We present results from detailed general relativistic simulations of stellar core collapse to a proto-neutron star, using two different microphysical nonzero-temperature nuclear equations of state as well as an approximate description of deleptonization during the collapse phase. Investigating a wide variety of rotation rates and profiles as well as masses of the progenitor stars and both equations of state, we confirm in this very general setup the recent finding that a generic gravitational wave burst signal is associated with core bounce, already known as type I in the literature. The previously suggested type II (or “multiple-bounce”) waveform morphology does not occur. Despite this reduction to a single waveform type, we demonstrate that it is still possible to constrain the progenitor and postbounce rotation based on a combination of the maximum signal amplitude and the peak frequency of the emitted gravitational wave burst. Our models include to sufficient accuracy the currently known necessary physics for the collapse and bounce phase of core-collapse supernovae, yielding accurate and reliable gravitational wave signal templates for gravitational wave data analysis. In addition, we assess the possibility of nonaxisymmetric instabilities in rotating nascent proto-neutron stars. We find strong evidence that in an iron core-collapse event the postbounce core cannot reach sufficiently rapid rotation to become subject to a classical bar-mode instability. However, many of our postbounce core models exhibit sufficiently rapid and differential rotation to become subject to the recently discovered dynamical instability at low rotation rates.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/2e750ebf48924ee75db77efaf5a2763082210210

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

In Geophysics

Citations in the corpus

Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, methodology): “More recently, Ott et al. (2007) [122, 183] and Dimmelmeier et al. (2008)[110] reported a 27In such a case, the ray-by-ray approximation would be not good.”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, background): “…the collapse and bounce of rapidly rotating iron cores and triaxial instabilities in the early post-bounce phase has long been studied in 2D (i.e. under the assumption of axisymme-try) and 3D (e.g. Dimmelmeier et al. 2007, 2008; Ott et al. 2007; Scheidegger et al. 2008; Abdikamalov et al. 2010).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “…parts of the evolution, have received a lot of interest, because a strong and characteristic signature could make them a promising source of a detectable gravitational-wave burst (for a review-like introduction to the subject and a nearly complete list of publications, see Dimmelmeier et al. 2008).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “This is expected based on previous work devoted to the GWs from rotating core collapse (Dimmelmeier et al. 2008; Abdikamalov et al. 2014; Richers et al. 2017; Torres-Forné et al. 2017).”
The astrophysical gravitational wave stochastic background (2011, methodology): “Based on simulated spectra of Dimmelmeier et al. (2008) and Sekiguchi & Shibata (2005), they considered different models with σ ∼ 500 and ν∗ = 200−800 Hz.”
Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA (2013, methodology): “…rate estimation based upon astrophysical population models and observations of Galactic BNS systems (e.g., Abadie et al. 2010b; Kim et al. 2013; Dominik et al. 2015; Vangioni et al. 2016; de Mink and Belczynski 2015; Eldridge et al. 2017; Belczynski et al. 2017; Kruckow et al. 2018) remains an…”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, result): “These qualitative features are in good agreement with what was found by previous extensive parameter studies of rotating core collapse (Ott et al. 2006; Dimmelmeier et al. 2008).”
Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo (2013, background): “For example, GWs emitted by various processes in core-collapse supernovae are anticipated to have relatively large bandwidths, between 150 – 500 Hz [48, 82, 113, 83], largely independent of detector configuration.”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, methodology): “…neutrino treatments such as a “deleptonization scheme” (Liebendörfer 2005) or a trapping scheme, but the applicability of such methods is naturally limited, e.g. to the collapse and bounce phase, (Ott et al. 2007a; Dimmelmeier et al. 2007a, 2008), or fast black hole formation (Ott et al. 2011).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, methodology): “…the ADM energy (or the total energy in the Newtonian case), the gravitational source term in the standard form of the energy Equation (7) used in Dimmelmeier et al. (2002a, 2005, 2008) does not have the form of a flux divergence, and therefore a standard finite-volume discretization will lead…”
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].”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “Current investigations, that focus on these early phases and rapid rotation, use 2D or 3D simulations, conformally-flat or full general relativity, finite-temperature nuclear equations of state (EOS), and deleptonization during collapse (Dimmelmeier et al. 2007, 2008; Ott et al. 2007).”