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
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Erratum: A critical assessment of turbulence models for 1D core-collapse supernova simulations (Monthly Notices of the Royal Astronomical Society (2019) 487 (5304-5323) DOI: 10.1086/185620)
Journal ArticleDOI
Binary-stripped Stars as Core-collapse Supernovae Progenitors
David Vartanyan,E. Laplace,Mathieu Renzo,Mathieu Renzo,Y. Götberg,Adam Burrows,Selma E. de Mink,Selma E. de Mink,Selma E. de Mink +8 more
TL;DR: In this article, a simulation study of single and binary-stripped stars with the same initial mass as candidates for core-collapse supernovae (11 −21 M ⊙) is presented, and it is shown that binary stripped stars core tend to have a smaller compactness parameter, with a more prominent, deeper silicon/oxygen interface, and explode preferentially to the corresponding single stars.
Journal ArticleDOI
Explosion Mechanism of Core-collapse Supernovae: Role of the Si/Si–O Interface
TL;DR: In this article , the authors present a simple criterion to predict the explodability of massive stars based on the density and entropy profiles before collapse, showing that if a pronounced density jump is present near the Si/Si-O interface, the star will likely explode.
Journal ArticleDOI
Three dimensional magnetorotational core-collapse supernova explosions of a 39 solar mass progenitor star
TL;DR: In this paper , three-dimensional simulations of magnetorotational supernovae using a 39'M' progenitor star with two different initial magnetic field strengths of 1010'G and 1012'G in the core were performed.
Peer Review
Black holes as the end state of stellar evolution: Theory and simulations
TL;DR: In this paper , the authors provide a concise overview of the evolutionary channels that may lead to black hole formation, including the classical route of iron core collapse, collapse due to pair instability in very massive stars, and the hypothetical scenario of supermassive star collapse.
References
More filters
Journal ArticleDOI
The Piecewise Parabolic Method (PPM) for Gas Dynamical Simulations
Phillip Colella,Paul R. Woodward +1 more
TL;DR: This work recognizes the need for additional dissipation in any higher-order Godunov method of this type, and introduces it in such a way so as not to degrade the quality of the results.
Journal ArticleDOI
Towards the ultimate conservative difference scheme. II. Monotonicity and conservation combined in a second-order scheme
TL;DR: Fromm's second-order scheme for integrating the linear convection equation is made monotonic through the inclusion of nonlinear feedback terms in this paper, where care is taken to keep the scheme in conservation form.
Journal ArticleDOI
Neutron Star Structure and the Equation of State
TL;DR: In this article, Buchdahl and Tolman showed that the moment of inertia and the binding energy of a neutron star are nearly universal functions of the star's compactness, which can be understood by considering two analytic, yet realistic, solutions of Einstein's equations.
Journal ArticleDOI
A Generalized equation of state for hot, dense matter
TL;DR: In this paper, an equation of state for hot, dense matter is presented in a form that is sufficiently rapid to use directly in hydrodynamical simulations, for example, in stellar collapse calculations.
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