scholarly journals Breaking stress of Coulomb crystals in the neutron star crust

2021 ◽  
Vol 2103 (1) ◽  
pp. 012002
Author(s):  
A A Kozhberov
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Zero Point ◽  
Breaking Stress ◽  
Electrostatic Energy ◽  
Zero Temperature ◽  
Coulomb Crystal ◽  
Neutron Star Crust ◽  
Crystal Model ◽  
Coulomb Crystals

Abstract It is generally accepted that the Coulomb crystal model can be used to describe matter in the neutron star crust. In [1] we study the properties of deformed Coulomb crystals and how their stability depends on the polarization of the electron background. The breaking stress in the crust σmax at zero temperature was calculated based on the analysis of the electrostatic energy and the phonon spectrum of the Coulomb crystal. In this paper, I briefly discuss the influence of zero-point, thermal contributions and the internal magnetic field on σmax.

scholarly journals Deformed crystals and torsional oscillations of neutron star crust

2020 ◽  
Vol 498 (4) ◽  
pp. 5149-5158 ◽  
Author(s):  
A A Kozhberov ◽  
D G Yakovlev
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Torsional Oscillation ◽  
Breaking Stress ◽  
Magnetic Star ◽  
Theoretical Modelling ◽  
Torsional Oscillations ◽  
Neutron Star Crust ◽  
Screening Parameter ◽  
Coulomb Crystals

ABSTRACT We study breaking stress of deformed Coulomb crystals in a neutron star crust, taking into account electron plasma screening of ion–ion interaction; calculated breaking stress is fitted as a function of electron screening parameter. We apply the results for analysing torsional oscillation modes in the crust of a non-magnetic star. We present exact analytical expression for the fundamental frequencies of such oscillations and show that the frequencies of all torsional oscillations are insensitive to the presence of the outer neutron star crust. The results can be useful in theoretical modelling of processes involving deformed Coulomb crystals in the crust of neutron stars, such as magnetic field evolution, torsional crustal, or magneto-elastic quasi-periodic oscillations of flaring soft gamma-ray repeaters, pulsar glitches. The applicability of the results to soft gamma-ray repeaters is discussed.

IN-MEDIUM ION MASS RENORMALIZATION AND LATTICE VIBRATIONS IN THE NEUTRON STAR CRUST

2004 ◽  
Vol 13 (01) ◽  
pp. 371-374 ◽  
Author(s):  
PIOTR MAGIERSKI
Keyword(s):  
Neutron Star ◽  
Specific Heat ◽  
Thermal Energy ◽  
Lattice Vibrations ◽  
Mass Renormalization ◽  
Coulomb Crystal ◽  
Neutron Star Crust

The inner crust of a neutron star consists of nuclei immersed in a superfluid neutron liquid. As these nuclei move through the fermionic medium they bring it into motion as well. As a result their mass is strongly renormalized and the spectrum of the ion lattice vibrations is significantly affected. Consequently we predict that the specific heat and the lattice thermal energy of the Coulomb crystal at these densities are noticeably modified.

scholarly journals On the Nature of Magnetars

2004 ◽  
Vol 218 ◽  
pp. 265-266
Author(s):  
Ya. N. Istomin
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Electromagnetic Fields ◽  
Gamma Ray ◽  
X Ray ◽  
Surface Magnetic Field ◽  
The Core ◽  
Neutron Star Crust ◽  
High Magnitude

The electromagnetic fields of magnetodipole radiation can penetrate to the conducting matter of a neutron star crust and create there electric currents and tangential magnetic fields of high magnitude. The solution obtained here has the form of surface magnetic field discontinuities propagating through the crust to the core. This model explains the phenomena of magnetars — Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars.

scholarly journals Conductivity of neutron star crust under superhigh magnetic fields and Ohmic decay of toroidal magnetic field of magnetar

2019 ◽  
Vol 68 (18) ◽  
pp. 180401
Author(s):  
Jian-Ling Chen ◽  
Hui Wang ◽  
Huan-Yu Jia ◽  
Zi-Wei Ma ◽  
Yong-Hong Li ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Toroidal Magnetic Field ◽  
Neutron Star Crust

scholarly journals Magnetic-field evolution with large-scale velocity circulation in a neutron-star crust

2020 ◽  
Vol 494 (3) ◽  
pp. 3790-3798 ◽  
Author(s):  
Yasufumi Kojima ◽  
Kazuki Suzuki
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Lorentz Force ◽  
Large Scale ◽  
Magnetic Energy ◽  
Fluid Motion ◽  
Navier Stokes Equation ◽  
Ohmic Dissipation ◽  
Neutron Star Crust ◽  
Field Evolution

ABSTRACT We examine the effects of plastic flow that appear in a neutron-star crust when a magnetic stress exceeds the threshold. The dynamics involved are described using the Navier–Stokes equation comprising the viscous-flow term, and the velocity fields for the global circulation are determined using quasi-stationary approximation. We simulate the magnetic-field evolution by taking into consideration the Hall drift, Ohmic dissipation, and fluid motion induced by the Lorentz force. The decrease in the magnetic energy is enhanced, as the energy converts to the bulk motion energy and heat. It is found that the bulk velocity induced by the Lorentz force has a significant influence in the low-viscosity and strong-magnetic-field regimes. This effect is crucial near magnetar surfaces.

scholarly journals Non-Stationary Accretion in Her X–1–like Systems

1996 ◽  
Vol 160 ◽  
pp. 537-538
Author(s):  
U. Geppert ◽  
V. Urpin
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Total Mass ◽  
Binary Systems ◽  
High Mass ◽  
Neutron Star Crust ◽  
Solid Region ◽  
Low Mass ◽  
Field Decay ◽  
The Magnetic Field

Accretion heats the neutron star crust thereby decreasing the electric conductivity in the solid region. This leads to a rapid field decay when the currents supporting the field are concentrated in the solid crust (Geppert & Urpin 1994, Urpin & Geppert 1995). Depending on the duration of the accretion phase and on the total mass accreted the field can be decreased by 3 − 4 orders of magnitude after 106− 107years. This mechanism explains the low magnetic fields of many pulsars entering binary systems.However, there exist both low–mass (e.g. Her X–1, 4U 1626–67) and high–mass (e.g. Cen X–3, SMC X–1) systems, where the neutron star deserves strong accretion and the magnetic field is still large.

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