scholarly journals Core-collapse Supernova Simulations and the Formation of Neutron Stars, Hybrid Stars, and Black Holes

2022 ◽  
Vol 924 (1) ◽  
pp. 38
Author(s):  
Takami Kuroda ◽  
Tobias Fischer ◽  
Tomoya Takiwaki ◽  
Kei Kotake
Keyword(s):  
Phase Transition ◽  
Shock Wave ◽  
Neutron Star ◽  
Strong Shock ◽  
Hadronic Matter ◽  
Detector Response ◽  
Core Collapse ◽  
Qcd Phase Transition ◽  
Supernova Explosions ◽  
Progenitor Stars

Abstract We investigate observable signatures of a first-order quantum chromodynamics (QCD) phase transition in the context of core-collapse supernovae. To this end, we conduct axially symmetric numerical relativity simulations with multi-energy neutrino transport, using a hadron–quark hybrid equation of state (EOS). We consider four nonrotating progenitor models, whose masses range from 9.6 to 70 M ⊙. We find that the two less-massive progenitor stars (9.6 and 11.2 M ⊙) show a successful explosion, which is driven by the neutrino heating. They do not undergo the QCD phase transition and leave behind a neutron star. As for the more massive progenitor stars (50 and 70 M ⊙), the proto-neutron star (PNS) core enters the phase transition region and experiences the second collapse. Because of a sudden stiffening of the EOS entering to the pure quark matter regime, a strong shock wave is formed and blows off the PNS envelope in the 50 M ⊙ model. Consequently the remnant becomes a quark core surrounded by hadronic matter, leading to the formation of the hybrid star. However, for the 70 M ⊙ model, the shock wave cannot overcome the continuous mass accretion and it readily becomes a black hole. We find that the neutrino and gravitational wave (GW) signals from supernova explosions driven by the hadron–quark phase transition are detectable for the present generation of neutrino and GW detectors. Furthermore, the analysis of the GW detector response reveals unique kHz signatures, which will allow us to distinguish this class of supernova explosions from failed and neutrino-driven explosions.

Signals of the QCD phase transition in core collapse supernovae—microphysical input and implications on the supernova dynamics

2010 ◽  
Vol 27 (11) ◽  
pp. 114102 ◽  
Author(s):  
T Fischer ◽  
I Sagert ◽  
M Hempel ◽  
G Pagliara ◽  
J Schaffner-Bielich ◽  
...  
Keyword(s):  
Phase Transition ◽  
Core Collapse ◽  
Qcd Phase Transition

scholarly journals The Supernova/GRB Connection

2005 ◽  
Vol 192 ◽  
pp. 403-410 ◽  
Author(s):  
P. Höflich ◽  
D. Baade ◽  
A. Khokhlov ◽  
L. Wang ◽  
J.C. Wheeler
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Central Region ◽  
Stellar Evolution ◽  
Axial Symmetry ◽  
Energy Deposition ◽  
Gamma Ray ◽  
Massive Stars ◽  
Core Collapse ◽  
Supernova Explosions

SummaryWe discuss the possible connection between supernova explosions (SN) and gamma-ray bursters (GRB) from the perspective of our current understanding of SN physics. Core collapse supernovae (SN) are the final stages of stellar evolution in massive stars during which the central region collapses, forms a neutron star (NS) or black hole, and the outer layers are ejected. Recent explosion scenarios assumed that the ejection is due to energy deposition by neutrinos into the envelope but detailed models do not produce powerful explosions. There is new and mounting evidence for an asphericity and, in particular, for axial symmetry in several supernovae which may be hard to reconcile within the spherical picture. The 3-D signatures are a key to understand core collapse supernovae and the GRB/SN connection. In this paper we study the effects and observational consequences of asymmetric explosions.

scholarly journals CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK-HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE

2011 ◽  
Vol 194 (2) ◽  
pp. 39 ◽  
Author(s):  
T. Fischer ◽  
I. Sagert ◽  
G. Pagliara ◽  
M. Hempel ◽  
J. Schaffner-Bielich ◽  
...  
Keyword(s):  
Phase Transition ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Hadron Phase ◽  
Supernova Explosions

scholarly journals Neutron Star Kicks Affected by Standing Accretion Shock Instability for Core-Collapse Supernovae

2011 ◽  
Vol 7 (S279) ◽  
pp. 337-338
Author(s):  
Wakana Iwakami Nakano ◽  
Kei Kotake ◽  
Naofumi Ohnishi ◽  
Shoichi Yamada ◽  
Keisuke Sawada
Keyword(s):  
Shock Wave ◽  
Neutron Star ◽  
Core Collapse ◽  
Random Perturbations ◽  
Initial Flow ◽  
Average Value ◽  
Different Types ◽  
Accretion Shock ◽  
Neutrino Luminosity ◽  
Proto Neutron Star

AbstractWe investigate a proto-neutron star kick velocity estimated from kinetic momentum of a flow around the proto-neutron star after the standing accretion shock instability grows. In this study, ten different types of random perturbations are imposed on the initial flow for each neutrino luminosity. We found that the kick velocities of proto-neutron star are widely distributed from 40 km s−1 to 180 km s−1 when the shock wave reaches 2000 km away from the center of the star. The average value of kick velocity is 115 km s−1, whose value is smaller than the observational ones. The kick velocities do not depend on the neutrino luminosity.

scholarly journals The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations

2019 ◽  
Vol 491 (2) ◽  
pp. 2715-2735 ◽  
Author(s):  
Adam Burrows ◽  
David Radice ◽  
David Vartanyan ◽  
Hiroki Nagakura ◽  
M Aaron Skinner ◽  
...  
Keyword(s):  
Neutron Star ◽  
Massive Star ◽  
State Of The Art ◽  
Mass Range ◽  
Core Collapse ◽  
Final States ◽  
Lower Mass ◽  
Core Collapse Supernova ◽  
Supernova Explosions ◽  
General Range

ABSTRACT We have conducted 19 state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the ‘compactness’ measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Ye = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.

Shock wave produced by hadron-quark phase transition in neutron star

2015 ◽  
Author(s):  
Luis Gustavo de Almeida ◽  
Sérgio José Barbosa Duarte ◽  
Hilário Rodrigues
Keyword(s):  
Phase Transition ◽  
Shock Wave ◽  
Neutron Star ◽  
Quark Phase

PHASE TRANSITION IN ROTATING NEUTRON STARS

2007 ◽  
Vol 16 (02n03) ◽  
pp. 333-339 ◽  
Author(s):  
G. F. MARRANGHELLO
Keyword(s):  
Phase Transition ◽  
Neutron Star ◽  
Neutron Stars ◽  
Strange Quark ◽  
Hadronic Matter ◽  
The Core ◽  
Mit Bag Model ◽  
Wave Emission ◽  
Linear Field ◽  
Field Theoretical Model

We review the properties of a phase transition from hadronic matter to deconfined strange quark matter in the core of neutron stars. The neutron star equation of state is computed using a non-linear field theoretical model and the MIT bag model. Rapidly rotating neutron star configurations are studied and the consequences of the conversion and a subsequently micro-collapse, such as gravitational wave emission and pulsar spin-up, are analyzed.

Sign in / Sign up

Export Citation Format

Share Document