scholarly journals Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers

2015 ◽  
Vol 92 (12) ◽  
Author(s):  
Kenta Kiuchi ◽  
Pablo Cerdá-Durán ◽  
Koutarou Kyutoku ◽  
Yuichiro Sekiguchi ◽  
Masaru Shibata
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Helmholtz Instability ◽  
Binary Neutron Star ◽  
Field Amplification

scholarly journals TURBULENT MAGNETIC FIELD AMPLIFICATION FROM SPIRAL SASI MODES: IMPLICATIONS FOR CORE-COLLAPSE SUPERNOVAE AND PROTO-NEUTRON STAR MAGNETIZATION

2012 ◽  
Vol 751 (1) ◽  
pp. 26 ◽  
Author(s):  
Eirik Endeve ◽  
Christian Y. Cardall ◽  
Reuben D. Budiardja ◽  
Samuel W. Beck ◽  
Alborz Bejnood ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Core Collapse ◽  
Field Amplification ◽  
Proto Neutron Star

scholarly journals SGRs and AXPs: Evidence for Delayed Amplification of Magnetic Field after Neutron Star Formation?

2009 ◽  
Vol 2009 ◽  
pp. 1-8 ◽  
Author(s):  
Denis Leahy ◽  
Rachid Ouyed
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Neutron Stars ◽  
Birth Rate ◽  
Massive Stars ◽  
Robust Estimator ◽  
High Magnetic Fields ◽  
Field Amplification ◽  
Kolmogorov Smirnov

We present new analysis of the birth rate of AXPs and SGRS and their associated SNRs. Using Kolmogorov-Smirnov statistics together with parametric fits based on a robust estimator, we find a birth rate of ∼1/(1000 years) for AXPs/SGRs and their associated SNRs. These high rates suggest that all massive stars (greater than ∼(23–32)M⊙) give rise to remnants with magnetar-like fields. Observations indicate a limited fraction of high magnetic fields in these progenitors; thus our study is suggestive of magnetic field amplification. Dynamo mechanisms during the birth of the neutron stars require spin rates much faster than either observations or theory indicate. We propose that massive stars produce neutron stars with normal (∼1012 G) magnetic fields, which are then amplified to1014-1015 G after a delay of hundreds of years. The amplification is speculated to be a consequence of color ferromagnetism and to occur with a delay after the neutron star core reaches quark deconfinement density (i.e., the quark-nova scenario). The delayed amplification allows one to interpret simultaneously the high birth rate and high magnetic fields of AXPs/SGRs and their link to massive stars.

scholarly journals Binary neutron star mergers and short gamma-ray bursts: Effects of magnetic field orientation, equation of state, and mass ratio

2016 ◽  
Vol 94 (6) ◽  
Author(s):  
Takumu Kawamura ◽  
Bruno Giacomazzo ◽  
Wolfgang Kastaun ◽  
Riccardo Ciolfi ◽  
Andrea Endrizzi ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Equation Of State ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Mass Ratio ◽  
Field Orientation ◽  
Magnetic Field Orientation ◽  
Binary Neutron Star

scholarly journals On the linear and non-linear evolution of the relativistic MHD Kelvin–Helmholtz instability in a magnetically polarized fluid

2019 ◽  
Vol 490 (3) ◽  
pp. 4183-4193
Author(s):  
Oscar M Pimentel ◽  
Fabio D Lora-Clavijo
Keyword(s):  
Magnetic Field ◽  
Gamma Ray ◽  
Magnetic Energy ◽  
Linear Regime ◽  
Helmholtz Instability ◽  
Linear Evolution ◽  
Field Amplification ◽  
Non Linear ◽  
Open Question ◽  
The Magnetic Field

ABSTRACT The origin and strength of the magnetic field in some systems like active galactic nuclei or gamma-ray bursts is still an open question in astrophysics. A possible mechanism to explain the magnetic field amplification is the Kelvin–Helmholtz instability, since it is able to transform the kinetic energy in a shear flow into magnetic energy. Through this work, we investigate the linear and non-linear effects produced by the magnetic susceptibility in the development of the Kelvin–Helmholtz instability in a relativistic plasma. The system under study consists of a plane interface separating two uniform fluids that move with opposite velocities. The magnetic field in the system is parallel to the flows and the susceptibility is assumed to be homogeneous, constant in time, and equal in both fluids. In particular, we analyse the instability in three different cases, when the fluids are diamagnetic, paramagnetic, and when the susceptibility is zero. We compute the dispersion relation in the linear regime and found that the interface between diamagnetic fluids is more stable than between paramagnetic ones. We check the analytical results with numerical simulations, and explore the effect of the magnetic polarization in the non-linear regime. We find that the magnetic field is more amplified in paramagnetic fluids than in diamagnetic ones. Surprisingly, the effect of the susceptibility in the amplification is stronger when the magnetization parameter is smaller. The results of our work make this instability a more efficient and effective amplification mechanism of seed magnetic fields when considering the susceptibility of matter.

scholarly journals Waveform systematics in the gravitational-wave inference of tidal parameters and equation of state from binary neutron-star signals

2021 ◽  
Vol 103 (12) ◽  
Author(s):  
Rossella Gamba ◽  
Matteo Breschi ◽  
Sebastiano Bernuzzi ◽  
Michalis Agathos ◽  
Alessandro Nagar
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Gravitational Wave ◽  
Binary Neutron Star
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