scholarly journals A new gravitational-wave signature of low-T/|W| instability in rapidly rotating stellar core collapse

2020 ◽  
Vol 493 (1) ◽  
pp. L138-L142 ◽  
Author(s):  
Shota Shibagaki ◽  
Takami Kuroda ◽  
Kei Kotake ◽  
Tomoya Takiwaki
Keyword(s):  
Gravitational Wave ◽  
Three Dimensional ◽  
Active Phase ◽  
Peak Frequency ◽  
Core Collapse ◽  
Time Modulation ◽  
General Relativistic ◽  
Wave Signature ◽  
The One ◽  
Strong Gravitational Wave

ABSTRACT We present results from a full general relativistic three-dimensional hydrodynamics simulation of rapidly rotating core collapse of a 70 M⊙ star with three-flavour spectral neutrino transport. We find a strong gravitational-wave (GW) emission that originates from the growth of the one- and two-armed spiral waves extending from the nascent proto-neutron star (PNS). The GW spectrogram shows several unique features that are produced by the non-axisymmetric instabilities. After bounce, the spectrogram first shows a transient quasi-periodic time modulation at ∼450 Hz. In the second active phase, it again shows the quasi-periodic modulation but with the peak frequency increasing with time, which continues until the final simulation time. From our detailed analysis, such features can be well explained by a combination of the so-called low-T/|W| instability and the PNS core contraction.

scholarly journals Three-dimensional core-collapse supernova simulations of massive and rotating progenitors

2020 ◽  
Vol 494 (4) ◽  
pp. 4665-4675 ◽  
Author(s):  
Jade Powell ◽  
Bernhard Müller
Keyword(s):  
Gravitational Wave ◽  
Rotation Axis ◽  
Three Dimensional ◽  
Low Frequency ◽  
High Mass ◽  
Core Collapse ◽  
Einstein Telescope ◽  
General Relativistic ◽  
Rapid Rotator ◽  
Helium Star

ABSTRACT We present 3D simulations of the core-collapse of massive rotating and non-rotating progenitors performed with the general relativistic neutrino hydrodynamics code coconut-fmt. The progenitor models include Wolf-Rayet stars with initial helium star masses of $39\, \mathrm{ M}_{\odot }$ and $20\, \mathrm{ M}_{\odot }$, and an $18\, \mathrm{ M}_{\odot }$ red supergiant. The $39\, \mathrm{ M}_{\odot }$ model is a rapid rotator, whereas the two other progenitors are non-rotating. Both Wolf-Rayet models produce healthy neutrino-driven explosions, whereas the red supergiant model fails to explode. By the end of the simulations, the explosion energies have already reached $1.1\times 10^{51}\, $ and $0.6\times 10^{51}\, \mathrm{erg}$ for the $39\, \mathrm{ M}_{\odot }$ and $20\, \mathrm{ M}_{\odot }$ model, respectively. They produce neutron stars of relatively high mass, but with modest kicks. Due to the alignment of the bipolar explosion geometry with the rotation axis, there is a relatively small misalignment of 30° between the spin and the kick in the rapidly rotating $39\, \mathrm{ M}_{\odot }$ model. For this model, we find that rotation significantly changes the dependence of the characteristic gravitational-wave frequency of the f-mode on the proto-neutron star parameters compared to the non-rotating case. Its gravitational-wave amplitudes would make it detectable out to almost 2 Mpc by the Einstein Telescope. The other two progenitors have considerably smaller detection distances, despite significant low-frequency emission in the most sensitive frequency band of current gravitational-wave detectors.

scholarly journals GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE

2013 ◽  
Vol 768 (2) ◽  
pp. 115 ◽  
Author(s):  
Christian D. Ott ◽  
Ernazar Abdikamalov ◽  
Philipp Mösta ◽  
Roland Haas ◽  
Steve Drasco ◽  
...  
Keyword(s):  
Three Dimensional ◽  
Core Collapse ◽  
General Relativistic

Non-exploding and exploding core-collapse supernova models and the multimessenger predictions

2019 ◽  
Vol 15 (S350) ◽  
pp. 267-273
Author(s):  
Kei Kotake ◽  
Takami Kuroda ◽  
Tomoya Takiwaki
Keyword(s):  
Black Hole ◽  
Massive Star ◽  
Three Dimensional ◽  
Core Collapse ◽  
Rapid Rotation ◽  
Core Collapse Supernova ◽  
Collapse Simulation ◽  
Collapse Model ◽  
General Relativistic ◽  
Proto Neutron Star

AbstractWe present results of full general relativistic (GR), three-dimensional (3D) core-collapse simulation of a massive star with multi-energy neutrino transport. Using a 70Mȯ zero-metallicity star, we show that the black-hole (BH) formation occurs at ∼ 300 ms after bounce. At a few ∼ 10 ms before the BH formation, we find that the stalled bounce shock is revived by neutrino heating from the forming hot proto-neutron star (PNS), which is aided by vigorous convection behind the shock. Our numerical results present the first evidence to validate the BH formation by the so-called fallback scenario. Furthermore we present results from a rapidly rotating core-collapse model of a 27Mȯ star that is trending towards an explosion. We point out that the correlated neutrino and gravitational-wave signatures, if detected, could provide a smoking-gun evidence of rapid rotation of the newly-born PNS.

scholarly journals Toward three-dimensional simulations of stellar core collapse with magnetic fields

2006 ◽  
Vol 2 (S239) ◽  
pp. 326-328
Author(s):  
M. Liebendörfer ◽  
S. Whitehouse ◽  
T. Fischer
Keyword(s):  
Neutrino Physics ◽  
Three Dimensional ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Net Energy ◽  
Stellar Core ◽  
Fluid Instabilities ◽  
General Relativistic ◽  
Accretion Shock ◽  
Neutrino Luminosity

AbstractIn spherical symmetry, very reliable models of stellar core collapse, bounce, and the postbounce phase can be constructed based on general relativistic Boltzmann neutrino transport. However, even if the time-integrated neutrino luminosity in the region between the surface of the protoneutron star and the stalled accretion shock is one or two orders of magnitude larger than the energy of a supernova explosion, it is generally accepted that the net energy transfer is not efficient enough to drive an explosion, unless the fluid instabilities in this regime are taken into account. Complementary to other groups, who are elaborating an extension of the accurate neutrino physics to axisymmetric simulations, we construct efficient parameterizations of the neutrino physics that enable three-dimensional magneto-hydrodynamics simulations that do not constrain the fluid instabilities by artificially imposed symmetries. We evaluate our approximations with respect to spherically symmetric Boltzmann neutrino transport, present preliminary MHD simulations with a resolution of 600 zones cubed, and illustrate the questions that can be addressed by this approach.

scholarly journals GENERAL-RELATIVISTIC THREE-DIMENSIONAL MULTI-GROUP NEUTRINO RADIATION-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE

2016 ◽  
Vol 831 (1) ◽  
pp. 98 ◽  
Author(s):  
Luke F. Roberts ◽  
Christian D. Ott ◽  
Roland Haas ◽  
Evan P. O’Connor ◽  
Peter Diener ◽  
...  
Keyword(s):  
Three Dimensional ◽  
Radiation Hydrodynamics ◽  
Core Collapse ◽  
Neutrino Radiation ◽  
General Relativistic
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