scholarly journals On the importance of the equation of state for the neutrino-driven supernova explosion mechanism

2011 ◽  
Vol 7 (S279) ◽  
pp. 397-398 ◽  
Author(s):  
Yudai Suwa
Keyword(s):  
Equation Of State ◽  
Supernova Explosion ◽  
Shock Propagation ◽  
Core Collapse ◽  
Two Dimensional ◽  
Core Collapse Supernova ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Explosion Mechanism ◽  
The Difference

AbstractWe present two-dimensional numerical simulations of core-collapse supernova including multi-energy neutrino radiative transfer. We aim to examine the influence of the equation of state (EOS) for the dense nuclear matter. We employ four sets of EOSs, namely, those by Lattimer and Swesty (LS) and Shen et al., which became standard EOSs in the core-collapse supernova community. We reconfirm that not every EOS produces an explosion in spherical symmetry, which is consistent with previous works. In two-dimensional simulations, we find that the structure of the accretion flow is significantly different between LS EOS and Shen EOS, inducing an even qualitatively different evolution of the shock wave, namely, the LS EOS leads to shock propagation beyond 2000 km from the center, while the Shen EOS shows only oscillations within 500 km. The possible origins of the difference are discussed.

scholarly journals Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

2019 ◽  
Vol 491 (4) ◽  
pp. 5376-5391 ◽  
Author(s):  
Sarah E Gossan ◽  
Jim Fuller ◽  
Luke F Roberts
Keyword(s):  
Acoustic Waves ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
The Core ◽  
Shock Region ◽  
Wave Heating ◽  
Post Shock ◽  
Explosion Mechanism ◽  
Proto Neutron Star

ABSTRACT Our understanding of the core-collapse supernova explosion mechanism is incomplete. While the favoured scenario is delayed revival of the stalled shock by neutrino heating, it is difficult to reliably compute explosion outcomes and energies, which depend sensitively on the complex radiation hydrodynamics of the post-shock region. The dynamics of the (non-)explosion depend sensitively on how energy is transported from inside and near the proto-neutron star (PNS) to material just behind the supernova shock. Although most of the PNS energy is lost in the form of neutrinos, hydrodynamic and hydromagnetic waves can also carry energy from the PNS to the shock. We show that gravity waves excited by core PNS convection can couple with outgoing acoustic waves that present an appreciable source of energy and pressure in the post-shock region. Using one-dimensional simulations, we estimate the gravity wave energy flux excited by PNS convection and the fraction of this energy transmitted upwards to the post-shock region as acoustic waves. We find wave energy fluxes near $10^{51}\, \mathrm{erg}\, \mathrm{s}^{-1}\,$ are likely to persist for $\sim \! 1\, \mathrm{s}$ post-bounce. The wave pressure on the shock may exceed $10{{\ \rm per\ cent}}$ of the thermal pressure, potentially contributing to shock revival and, subsequently, a successful and energetic explosion. We also discuss how future simulations can better capture the effects of waves, and more accurately quantify wave heating rates.

scholarly journals The Core-Collapse Supernova Explosion Mechanism

2016 ◽  
Vol 12 (S329) ◽  
pp. 17-24 ◽  
Author(s):  
Bernhard Müller
Keyword(s):  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
The Core ◽  
Supernova Explosions ◽  
Explosion Mechanism ◽  
Standing Problem

AbstractThe explosion mechanism of core-collapse supernovae is a long-standing problem in stellar astrophysics. We briefly outline the main contenders for a solution and review recent efforts to model core-collapse supernova explosions by means of multi-dimensional simulations. Focusing on the neutrino-driven mechanism, we summarize currents efforts to predict supernova explosion and remnant properties.

scholarly journals Stripped-envelope core-collapse supernova 56Ni masses

2020 ◽  
Vol 641 ◽  
pp. A177 ◽  
Author(s):  
N. Meza ◽  
J. P. Anderson
Keyword(s):  
Systematic Errors ◽  
Power Source ◽  
Radioactive Material ◽  
Estimation Methods ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Explosion Mechanism ◽  
The Difference ◽  
Uniform Manner ◽  
Lower Limits

Context. The mass of synthesised radioactive material is an important power source for all supernova (SN) types. In addition, the difference of 56Ni yields statistics are relevant to constrain progenitor paths and explosion mechanisms. Aims. Here, we re-estimate the nucleosynthetic yields of 56Ni for a well-observed and well-defined sample of stripped-envelope SNe (SE-SNe) in a uniform manner. This allows us to investigate whether the observed hydrogen-rich–stripped-envelope (SN II–SE SN) 56Ni separation is due to real differences between these SN types or because of systematic errors in the estimation methods. Methods. We compiled a sample of well-observed SE-SNe and measured 56Ni masses through three different methods proposed in the literature: first, the classic “Arnett rule”; second the more recent prescription of Khatami & Kasen (2019, ApJ, 878, 56) and third using the tail luminostiy to provide lower limit 56Ni masses. These SE-SN distributions were then compared to those compiled in this article. Results. Arnett’s rule, as previously shown, gives 56Ni masses for SE-SNe that are considerably higher than SNe II. While for the distributions calculated using both the Khatami & Kasen (2019, ApJ, 878, 56) prescription and Tail 56Ni masses are offset to lower values than “Arnett values”, their 56Ni distributions are still statistically higher than that of SNe II. Our results are strongly driven by a lack of SE-SN with low 56Ni masses, that are, in addition, strictly lower limits. The lowest SE-SN 56Ni mass in our sample is of 0.015 M⊙, below which are more than 25% of SNe II. Conclusions. We conclude that there exist real, intrinsic differences in the mass of synthesised radioactive material between SNe II and SE-SNe (types IIb, Ib, and Ic). Any proposed current or future CC SN progenitor scenario and explosion mechanism must be able to explain why and how such differences arise or outline a bias in current SN samples yet to be fully explored.

scholarly journals Two‐dimensional, Time‐dependent, Multigroup, Multiangle Radiation Hydrodynamics Test Simulation in the Core‐Collapse Supernova Context

2004 ◽  
Vol 609 (1) ◽  
pp. 277-287 ◽  
Author(s):  
Eli Livne ◽  
Adam Burrows ◽  
Rolf Walder ◽  
Itamar Lichtenstadt ◽  
Todd A. Thompson
Keyword(s):  
Time Dependent ◽  
Radiation Hydrodynamics ◽  
Core Collapse ◽  
Two Dimensional ◽  
Core Collapse Supernova ◽  
The Core

scholarly journals Nuclear equation of state and neutron star cooling

2017 ◽  
Vol 26 (04) ◽  
pp. 1750015 ◽  
Author(s):  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Evolution ◽  
Observation Data ◽  
Nuclear Equation Of State ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Nuclear Models

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models of dense nuclear matter. We focus on the effects of uncertainties originated from the nuclear models, the composition of elements in the envelope region, and the formation of superfluidity in the core and the crust of neutron stars. Discovery of [Formula: see text] neutron stars PSR J1614−2230 and PSR J0343[Formula: see text]0432 has triggered the revival of stiff nuclear equation of state at high densities. In the meantime, observation of a neutron star in Cassiopeia A for more than 10 years has provided us with very accurate data for the thermal evolution of neutron stars. Both mass and temperature of neutron stars depend critically on the equation of state of nuclear matter, so we first search for nuclear models that satisfy the constraints from mass and temperature simultaneously within a reasonable range. With selected models, we explore the effects of element composition in the envelope region, and the existence of superfluidity in the core and the crust of neutron stars. Due to uncertainty in the composition of particles in the envelope region, we obtain a range of cooling curves that can cover substantial region of observation data.

scholarly journals A successful 3D core-collapse supernova explosion model

2018 ◽  
Vol 482 (1) ◽  
pp. 351-369 ◽  
Author(s):  
David Vartanyan ◽  
Adam Burrows ◽  
David Radice ◽  
M Aaron Skinner ◽  
Joshua Dolence
Keyword(s):  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova
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