scholarly journals Three‐Dimensional Simulations of Standing Accretion Shock Instability in Core‐Collapse Supernovae

2008 ◽  
Vol 678 (2) ◽  
pp. 1207-1222 ◽  
Author(s):  
Wakana Iwakami ◽  
Kei Kotake ◽  
Naofumi Ohnishi ◽  
Shoichi Yamada ◽  
Keisuke Sawada
Keyword(s):  
Three Dimensional ◽  
Core Collapse ◽  
Accretion Shock ◽  
Three Dimensional Simulations

scholarly journals The impact of fallback on the compact remnants and chemical yields of core-collapse supernovae

2020 ◽  
Vol 495 (4) ◽  
pp. 3751-3762 ◽  
Author(s):  
Conrad Chan ◽  
Bernhard Müller ◽  
Alexander Heger
Keyword(s):  
Binding Energy ◽  
Gamma Ray ◽  
Three Dimensional ◽  
Explosion Energy ◽  
Core Collapse ◽  
Abundance Patterns ◽  
Small Set ◽  
The Impact ◽  
Disc Formation ◽  
Three Dimensional Simulations

ABSTRACT Fallback in core-collapse supernovae plays a crucial role in determining the properties of the compact remnants and of the ejecta composition. We perform three-dimensional simulations of mixing and fallback for selected non-rotating supernova models to study how explosion energy and asymmetries correlate with the remnant mass, remnant kick, and remnant spin. We find that the strongest kick and spin are imparted by partial fallback in an asymmetric explosion. Black hole (BH) kicks of several hundred $\mathrm{km}\, \mathrm{s}^{-1}$ and spin parameters of $\mathord {\sim }0.25$ can be obtained in this scenario. If the initial explosion energy barely exceeds the envelope binding energy, stronger fallback results, and the remnant kick and spin remain small. If the explosion energy is high with respect to the envelope binding energy, there is little fallback with a small effect on the remnant kick, but the spin-up by fallback can be substantial. For a non-rotating $12\, \mathrm{M}_\odot$ progenitor, we find that the neutron star is spun up to millisecond periods. The high specific angular momentum of the fallback material can also lead to disc formation around BHs. Fallback may thus be a pathway towards millisecond-magnetar or collapsar-type engines for hypernovae and gamma-ray bursts that does not require rapid progenitor rotation. Within our small set of simulations, none reproduced the peculiar layered fallback necessary to explain the metal-rich iron-poor composition of many carbon-enhanced metal-poor (CEMP) stars. Models with different explosion energy and different realizations of asymmetries may, however, be compatible with CEMP abundance patterns.

scholarly journals The mechanism(s) of core-collapse supernovae

2017 ◽  
Vol 375 (2105) ◽  
pp. 20160271 ◽  
Author(s):  
Sean M. Couch
Keyword(s):  
Massive Stars ◽  
Three Dimensional ◽  
Short Review ◽  
Core Collapse ◽  
The Impact ◽  
Three Dimensional Simulations

Core-collapse supernovae (CCSNe) are the explosions that attend the deaths of massive stars. Despite decades of research, several aspects of the mechanism that drives these explosions remain uncertain and the subjects of continued investigation. In this short review, I will give an overview of the CCSN mechanism and current research in the field. In particular, I will focus on recent results from three-dimensional simulations and the impact of turbulence and detailed non-spherical progenitor structure on CCSNe. This contribution is based on a talk given at the ‘Bridging the Gap’ workshop at Chicheley Hall on 2 June 2016. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.

scholarly journals Spectropolarimetry of stripped-envelope supernovae: observations and modelling

2017 ◽  
Vol 375 (2105) ◽  
pp. 20160273 ◽  
Author(s):  
Masaomi Tanaka
Keyword(s):  
Large Scale ◽  
Massive Stars ◽  
Three Dimensional ◽  
Core Collapse ◽  
Ion Distribution ◽  
Typical Size ◽  
Cassiopeia A ◽  
Accretion Shock

Spectropolarimetry is one of the most powerful methods to study the multi-dimensional geometry of supernovae (SNe). We present a brief summary of the spectropolarimetric observations of stripped-envelope core-collapse SNe. Observations indicate that stripped-envelope SNe generally have a non-axisymmetric ion distribution in the ejecta. Three-dimensional clumpy geometry nicely explains the observed properties. A typical size of the clumps deduced from observations is relatively large: 25% of the photosphere. Such a large-scale clumpy structure is similar to that observed in Cassiopeia A, and suggests that large-scale convection or standing accretion shock instability takes place at the onset of the explosion. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.

scholarly journals THREE-DIMENSIONAL SIMULATIONS OF RAYLEIGH-TAYLOR MIXING IN CORE-COLLAPSE SUPERNOVAE

2010 ◽  
Vol 723 (1) ◽  
pp. 353-363 ◽  
Author(s):  
C. C. Joggerst ◽  
A. Almgren ◽  
S. E. Woosley
Keyword(s):  
Three Dimensional ◽  
Core Collapse ◽  
Three Dimensional Simulations
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