Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors
Bernhard Müller,Thomas M. Tauris,Alexander Heger,Projjwal Banerjee,Yong Zhong Qian,Jade Powell,Conrad Chan,Norbert Langer,Norbert Langer +8 more
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In this paper, a suite of seven 3D supernova simulations of non-rotating low-mass progenitors using multi-group neutrino transport is presented, where the mass outflow rate already exceeds the accretion rate onto the proto-neutron star and the mass and angular momentum of the compact remnant have closely approached their final value, barring the possibility of later fallback.Abstract:
We present a suite of seven 3D supernova simulations of non-rotating low-mass progenitors using multi-group neutrino transport. Our simulations cover single star progenitors with zero-age main sequence masses between $9.6 M_\odot$ and $12.5 M_\odot$ and (ultra)stripped-envelope progenitors with initial helium core masses between $2.8 M_\odot$ and $3.5 M_\odot$. We find explosion energies between $0.1\,\mathrm{Bethe}$ and $0.4\,\mathrm{Bethe}$, which are still rising by the end of the simulations. Although less energetic than typical events, our models are compatible with observations of less energetic explosions of low-mass progenitors. In six of our models, the mass outflow rate already exceeds the accretion rate onto the proto-neutron star, and the mass and angular momentum of the compact remnant have closely approached their final value, barring the possibility of later fallback. While the proto-neutron star is still accelerated by the gravitational tug of the asymmetric ejecta, the acceleration can be extrapolated to obtain estimates for the final kick velocity. We obtain gravitational neutron star masses between $1.22 M_\odot$ and $1.44 M_\odot$, kick velocities between $11\, \mathrm{km}\, \mathrm{s}^{-1}$ and $695\, \mathrm{km}\, \mathrm{s}^{-1}$, and spin periods from $20\, \mathrm{ms}$ to $2.7\,\mathrm{s}$, which suggests that typical neutron star birth properties can be naturally obtained in the neutrino-driven paradigm. We find a loose correlation between the explosion energy and the kick velocity. There is no indication of spin-kick alignment, but a correlation between the kick velocity and the neutron star angular momentum, which needs to be investigated further as a potential point of tension between models and observations.read more
Citations
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Three-dimensional core-collapse supernova simulations of massive and rotating progenitors
Jade Powell,Bernhard Müller +1 more
TL;DR: In this article, the core-collapse of massive rotating and non-rotating progenitors is simulated with the general relativistic neutrino hydrodynamics code CoCoNuT-FMT.
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Self-consistent 3D Supernova Models From −7 Minutes to +7 s: A 1-bethe Explosion of a ∼19 M ⊙ Progenitor
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TL;DR: In this article, fast-rising blue optical transients (FBOTs) and the brightest event of the class, AT2018cow, result from an electron-capture collapse to a neutron star following the merger of a massive ONeMg white dwarf with another WD.
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A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations
TL;DR: In this article, the first systematic study of proto-neutron star convection in three dimensions (3D) based on the latest numerical Fornax models of core-collapse supernova (CCSN) is presented.
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Astrophysics with the Laser Interferometer Space Antenna
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TL;DR: In this paper , a review of the current knowledge in three main source classes for LISA is reviewed; ultracompact stellar-mass binaries, massive black hole binaries, and extreme or intermediate mass ratio inspirals.
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