Toward Gravitational Wave Signals from Realistic Core-Collapse Supernova Models

By E. Mueller, Markus Rampp, R. Buras, Hans-Thomas Janka, D. Shoemaker. 2003

146 citations recorded by the source corpus.

We have computed the gravitational wave signal from supernova core collapse by using the most realistic input physics available at present. We start from state-of-the-art progenitor models of rotating and nonrotating massive stars and simulate the dynamics of their core collapse by integrating the equations of axisymmetric hydrodynamics, together with the Boltzmann equation for the neutrino transport, including an elaborate description of neutrino interactions, and a realistic equation of state. Using the Einstein quadrupole formula we compute the quadrupole wave amplitudes, the Fourier wave spectra, the amount of energy radiated in the form of gravitational waves, and the signal-to-noise ratios for the Laser Interferometer Gravitational-Wave Observatory (LIGO) I and the tuned Advanced LIGO (LIGO II) interferometers resulting from both nonradial mass motion and anisotropic neutrino emission. The simulations demonstrate that the dominant contribution to the gravitational wave signal is produced by neutrino-driven convection behind the supernova shock. For stellar cores rotating at the extreme of current stellar evolution predictions, the core bounce signal is detectable (S/N ≳ 7) with LIGO II for a supernova up to a distance of ~5 kpc, whereas the signal from postshock convection is observable (S/N ≳ 7) with LIGO II up to a distance of ~100 kpc and with LIGO I to a distance of ~5 kpc. If the core is nonrotating, its gravitational wave emission can be measured with LIGO II up to a distance of ~15 kpc (S/N ≳ 8), while the signal from the Ledoux convection in the deleptonizing nascent neutron star can be detected up to a distance of ~10 kpc (S/N ≳ 8). Both kinds of signals are generically produced by convection in any core-collapse supernova.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/698014a838523344813cda293ddc2ba9c9166a63

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Citations in the corpus

Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, methodology): “the panel) and their spectra (sum of ma tter and neutrino (bottom left) and contribution only from neutrino GWs (bottom right)) for a rotating model (s15r) of 15 M⊙ progenitor in Mu¨ller et al. (2004)[120]. The insert in the top left panel shows an enlargement of the signal near bounce, which comes ”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, unknown): “1 in Müller et al. 2004 and Sect.”
The astrophysical gravitational wave stochastic background (2011, methodology): “Buonanno et al. (2005) estimated the background produced by both ordinary supernovae and pop III stars using different numerical models of the GW waveform (Fryer et al. 2004; Müller et al. 2004).”
The Spin Periods and Rotational Profiles of Neutron Stars at Birth (2005, unknown): “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).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, methodology): “…gravitationalwave strain h(t) for the matter signal are of the order of several 10−22 for a source at a distance of 10 kpc, and the dominant peak may be marginally observable with LIGO I in the case of a Galactic supernova (for a detailed discussion of measurement aspects, see Müller et al. 2004).”
The physics of core-collapse supernovae (2005, methodology): “Measurements from a future supernova in the Milky Wa”
Science case for the Einstein telescope (2019, background): “Besides, the Standing Accretion Shock Instability (SASI) [127, 128] which is an instability of the supernova shock wave itself is expected, in conjunction with turbulence, to modulate the accretion flow, to excite the proto-neutro star high frequency oscillation modes as well as to generate low freq”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, methodology): “The initial rotation profile that we employ was discussed in detail by Müller et al. (2004) (see also Fig.”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, unknown): “3 and in Müller et al. (2004).”
Explosion mechanism, neutrino burst and gravitational wave in core-collapse supernovae (2005, methodology): “As a realistic EOS, Lattimer-Swesty (LS) EOS [209] has been used in recent papers discussing gravitational radiations from the rotational core collapse [288, 269].”