Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae

By Andreas Marek, Hans-Thomas Janka, E. Mueller. 2008

159 citations recorded by the source corpus.

We present two-dimensional (axisymmetric) neutrino-hydrodynamic simulations of the long-time accretion phase of a 15 Mprogen- itor star after core bounce and before the launch of a supernova explosion, when non-radial hydrodynamic instabilities like convection occur in different regions of the collapsing stellar core and the standing accretion shock instability (SASI) leads to large-amplitude os- cillations of the stalled shock with a period of tens of milliseconds. Our simulations were performed with the Prometheus-Vertex code, which includes a multi-flavor, energy-dependent neutrino transport scheme and employs an effective relativistic gravitational potential. Testing the influence of a stiff and a soft equation of state for hot neutron star matter, we find that the non-radial mass motions in the supernova core impose a time variability on the neutrino and gravitational-wave signals with larger amplitudes, as well as higher frequencies in the case of a more compact nascent neutron star. After the prompt shock-breakout burst of electron neutrinos, a more compact accreting remnant produces higher neutrino luminosities and higher mean neutrino energies. The observ- able neutrino emission in the SASI sloshing direction exhibits a modulation of several ten percent in the luminosities and around 1 MeV in the mean energies with most power at typical SASI frequencies between roughly 20 and 100 Hz. The modulation is caused by quasi-periodic variations in the mass accretion rate of the neutron star in each hemisphere. At times later than ∼50-100 ms after bounce, the gravitational-wave amplitude is dominated by the growing low-frequency (<200 Hz) signal associated with anisotropic neutrino emission. A high-frequency wave signal results from nonradial gas flows in the outer layers of the anisotropically accreting neutron star. Right after bounce such nonradial mass motions occur due to prompt post-shock convection in both considered cases and contribute mostly to the early wave production around 100 Hz. Later they are instigated by the SASI and by convective overturn that vigorously stir the neutrino-heating and cooling layers, and also by convective activity developing below the neutrinosphere. The gravitational-wave power then peaks at about 300-800 Hz, connected to changes in the mass quadrupole moment on a timescale of milliseconds. Distinctively higher spectral frequencies originate from the more compact and more rapidly contracting neutron star. Both the neutrino and gravitational-wave emission therefore carry information that is characteristic of the properties of the nuclear equation of state in the hot remnant. The detectability of the SASI effects in the neutrino and gravitational-wave signals is briefly discussed.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8acd660c312149564d4d471d1cc51dc796eac629

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Citations in the corpus

SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, background): “Quasi-periodic variations of the accretion flow onto the neutron star due to SASI shock oscillations may also cause fluctuations of the radiated neutrino luminosities and mean energies (Marek et al. 2009; Ott et al. 2008; Brandt et al. 2011).”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, methodology): “Moreover, as demonstrated by previous work (Kotake et al. 2009, 2011; E. Müller et al. 2012; Marek et al. 2009; Yakunin et al. 2010), GW emission due to asymmetric neutrino emission occurs at too low frequencies to be relevant for earthbound detectors such as Advanced LIGO (Harry (for the LIGO…”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “Since our treatment of the microphysics and the neutrino transport is on par with previous works on the GW signal from 2D simulations (Marek et al. 2009; Yakunin et al. 2010; M¨uller et al. 2013; Yakunin et al. 2015), we were in the position to conduct a meaningful comparison of GW emission in 2D…”
What can be learned from a future supernova neutrino detection (2017, methodology): “Monte Carlo realization (red histogram) and reconstructed fit (blue line) for the photon counts per time bin at IceCube, based on the benchmark core-collapse distance of 10 kpc and using the simulation of the Garching group [43].”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “This figure reveals the usual behavior during the postbounce accretion phase (compare, e.g., with results by Marek & Janka 2009; Marek et al. 2009; Janka et al. 2012).”
The Nuclear Symmetry Energy (2016, methodology): “Furthermore it has been found that it is essential to perform the simulations in two or, better, three dimensions (rather than in spherical symmetry) to obtain a successful explosion, at least for the larger masses [122, 123, 124].”
CORE-COLLAPSE SUPERNOVA EQUATIONS OF STATE BASED ON NEUTRON STAR OBSERVATIONS (2012, background): “To tackle the impact of the EOS on the explosion mechanism, multi-dimensional simulations are necessary, see e.g. Marek et al. (2009).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “Such fast variations in the postbounce luminosity evolution 5 have been already found in previous 2D studies (e.g., Ott et al. (2008); Marek et al. (2009)).”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, unknown): “…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. 2014; Yakunin et al. 2015; Morozova et al.…”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “The acoustic mechanism relies on the revival of the stalled bounce shock by the energy deposition via the acoustic waves that the oscillating protoneutron stars (PNSs) would emit in a much delayed phase (∼ 1 second) compared to the conventional neutrino-heating mechanism (∼ 300− 600 milliseconds).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “Empirically it has been found that when this ratio reaches 1 an explosion is expected (Marek et al. 2009; O’Connor & Couch 2018).”
Symmetry energy impact in simulations of core-collapse supernovae (2013, methodology): “trino heating and cooling, dominate the post bounce evolution. Consequently, dierences to the spherical case can be very large and the above reported dierences due to the nuclear EOS may be altered [74,12,75]. Currently available multi-dimensional supernova simulations indicate a structural feedback”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “This signal is usually associated with the surface g-modes of the newly formed proto-neutron star (PNS) excited by the downflows from the postshock convection region or from convection inside the PNS itself (Murphy et al. 2009; Marek et al. 2009; Müller et al. 2013).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, methodology): “The evolution in frequency from∼100 Hz just after bounce to larger frequencies at later times agrees with the results of Marek et al. (2009).”