scholarly journals Gravitational radiation from rotational core collapse: Effects of magnetic fields and realistic equations of state

2004 ◽  
Vol 69 (12) ◽  
Author(s):  
Kei Kotake ◽  
Shoichi Yamada ◽  
Katsuhiko Sato ◽  
Kohsuke Sumiyoshi ◽  
Hiroyuki Ono ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Gravitational Radiation ◽  
Equations Of State ◽  
Core Collapse

scholarly journals Gravitational Radiation from Standing Accretion Shock Instability in Core‐Collapse Supernovae

2007 ◽  
Vol 655 (1) ◽  
pp. 406-415 ◽  
Author(s):  
Kei Kotake ◽  
Naofumi Ohnishi ◽  
Shoichi Yamada
Keyword(s):  
Gravitational Radiation ◽  
Core Collapse ◽  
Accretion Shock

NEUTRINO PROCESSES IN STRONG MAGNETIC FIELDS AND SUPERNOVA PHYSICS

2005 ◽  
Vol 20 (32) ◽  
pp. 2435-2447
Author(s):  
HUAIYU DUAN
Keyword(s):  
Magnetic Fields ◽  
Charged Particles ◽  
Core Collapse ◽  
Strong Magnetic Fields

Strong magnetic fields are suspected to exist in some core-collapse supernovae, which would affect the neutrino processes such as νe+n ⇌ e-+p and [Formula: see text]. We briefly review the motion of charged particles in the presence of magnetic fields and the changes of the above processes induced by magnetic fields. We also discuss the implications of these changes for supernova physics in the context of neutrino-driven explosion.

The effects of superhigh magnetic fields on the equations of state of neutron stars

2015 ◽  
Vol 336 (8-9) ◽  
pp. 866-870 ◽  
Author(s):  
Z. F. Gao ◽  
N. Wang ◽  
Y. XU ◽  
H. Shan ◽  
X.-D. Li
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
Equations Of State

scholarly journals How to form a millisecond magnetar? Magnetic field amplification in protoneutron stars

2017 ◽  
Vol 12 (S331) ◽  
pp. 119-124 ◽  
Author(s):  
Jérôme Guilet ◽  
Ewald Müller ◽  
Hans-Thomas Janka ◽  
Tomasz Rembiasz ◽  
Martin Obergaulinger ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Gamma Ray ◽  
Core Collapse ◽  
Magnetorotational Instability ◽  
Strong Magnetic Fields ◽  
Physical Conditions ◽  
Field Amplification ◽  
Magnetic Prandtl Number ◽  
Protoneutron Stars

AbstractExtremely strong magnetic fields of the order of 1015G are required to explain the properties of magnetars, the most magnetic neutron stars. Such a strong magnetic field is expected to play an important role for the dynamics of core-collapse supernovae, and in the presence of rapid rotation may power superluminous supernovae and hypernovae associated to long gamma-ray bursts. The origin of these strong magnetic fields remains, however, obscure and most likely requires an amplification over many orders of magnitude in the protoneutron star. One of the most promising agents is the magnetorotational instability (MRI), which can in principle amplify exponentially fast a weak initial magnetic field to a dynamically relevant strength. We describe our current understanding of the MRI in protoneutron stars and show recent results on its dependence on physical conditions specific to protoneutron stars such as neutrino radiation, strong buoyancy effects and large magnetic Prandtl number.

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