The Three Dimensional MHD Effects For Core Collapse Supernova Explosion

2008 ◽  
Author(s):  
Hayato Mikami ◽  
Yuji Sato ◽  
Tomoaki Matsumoto ◽  
Tomoyuki Hanawa ◽  
Ye-Fei Yuan ◽  
...  
Keyword(s):  
Three Dimensional ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova

scholarly journals Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

2021 ◽  
Vol 921 (2) ◽  
pp. 113
Author(s):  
Michael A. Sandoval ◽  
W. Raphael Hix ◽  
O. E. Bronson Messer ◽  
Eric J. Lentz ◽  
J. Austin Harris
Keyword(s):  
Three Dimensional ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Isotopic Species

scholarly journals Towards an understanding of the resolution dependence of Core-Collapse Supernova simulations

2019 ◽  
Vol 490 (4) ◽  
pp. 4622-4637 ◽  
Author(s):  
Hiroki Nagakura ◽  
Adam Burrows ◽  
David Radice ◽  
David Vartanyan
Keyword(s):  
Spatial Resolution ◽  
State Of The Art ◽  
Three Dimensional ◽  
Core Collapse ◽  
Turbulent Stress ◽  
Critical Aspect ◽  
Core Collapse Supernova ◽  
Nuclear Equation Of State ◽  
Turbulent Eddies ◽  
Polar Grid

ABSTRACT Using our new state-of-the-art core-collapse supernova (CCSN) code Fornax, we explore the dependence upon spatial resolution of the outcome and character of three-dimensional (3D) supernova simulations. For the same 19 M⊙ progenitor star, energy and radial binning, neutrino microphysics, and nuclear equation of state, changing only the number of angular bins in the θ and ϕ directions, we witness that our lowest resolution 3D simulation does not explode. However, when jumping progressively up in resolution by factors of two in each angular direction on our spherical-polar grid, models then explode, and explode slightly more vigorously with increasing resolution. This suggests that there can be a qualitative dependence of the outcome of 3D CCSN simulations upon spatial resolution. The critical aspect of higher spatial resolution is the adequate capturing of the physics of neutrino-driven turbulence, in particular its Reynolds stress. The greater numerical viscosity of lower resolution simulations results in greater drag on the turbulent eddies that embody turbulent stress, and, hence, in a diminution of their vigor. Turbulent stress not only pushes the temporarily stalled shock further out, but bootstraps a concomitant increase in the deposited neutrino power. Both effects together lie at the core of the resolution dependence we observe.

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

scholarly journals A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations

2020 ◽  
Vol 492 (4) ◽  
pp. 5764-5779 ◽  
Author(s):  
Hiroki Nagakura ◽  
Adam Burrows ◽  
David Radice ◽  
David Vartanyan
Keyword(s):  
Neutron Star ◽  
Systematic Study ◽  
Three Dimensional ◽  
Three Dimensions ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Tau Neutrinos ◽  
The Impact ◽  
Proto Neutron Star

ABSTRACT This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical fornax models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, $\bar{\nu }_{\mu }$, and $\bar{\nu }_{\tau }$ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.

scholarly journals THREE-DIMENSIONAL SIMULATION OF A ROTATING CORE-COLLAPSE SUPERNOVA

2015 ◽  
Vol 30 (2) ◽  
pp. 481-483
Author(s):  
KO NAKAMURA ◽  
TAKAMI KURODA ◽  
TOMOYA TAKIWAKI ◽  
KEI KOTAKE
Keyword(s):  
Three Dimensional ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Dimensional Simulation

scholarly journals DENSE IRON EJECTA AND CORE-COLLAPSE SUPERNOVA EXPLOSION IN THE YOUNG SUPERNOVA REMNANT G11.2-0.3

2009 ◽  
Vol 703 (1) ◽  
pp. L81-L85 ◽  
Author(s):  
Dae-Sik Moon ◽  
Bon-Chul Koo ◽  
Ho-Gyu Lee ◽  
Keith Matthews ◽  
Jae-Joon Lee ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Young Supernova Remnant

scholarly journals Gravitational wave signatures ofab initiotwo-dimensional core collapse supernova explosion models for12–25  M⊙stars

2015 ◽  
Vol 92 (8) ◽  
Author(s):  
Konstantin N. Yakunin ◽  
Anthony Mezzacappa ◽  
Pedro Marronetti ◽  
Shin’ichirou Yoshida ◽  
Stephen W. Bruenn ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
M Stars
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