Exotic Nuclear Rod Formation Induced by Superfluid Vortices in Neutron Star Crusts

1997 ◽  
Vol 489 (2) ◽  
pp. 848-864 ◽  
Author(s):  
Yuko S. Mochizuki ◽  
Kazuhiro Oyamatsu ◽  
Takeo Izuyama
Keyword(s):  
Neutron Star ◽  
Superfluid Vortices

scholarly journals Modelling strains and stresses in continuously stratified rotating neutron stars

2019 ◽  
Author(s):  
E Giliberti ◽  
G Cambiotti ◽  
M Antonelli ◽  
P M Pizzochero
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Adiabatic Index ◽  
Practical Application ◽  
Polytropic Equation ◽  
Vela Pulsar ◽  
Superfluid Vortices ◽  
The Impact ◽  
Stellar Configuration

Abstract We introduce a Newtonian model for the deformations of a compressible, auto-gravitating and continuously stratified neutron star. The present framework can be applied to a number of astrophysical scenarios as it allows to account for a great variety of loading forces. In this first analysis, the model is used to study the impact of a frozen adiabatic index in the estimate of rotation-induced deformations: we assume a polytropic equation of state for the matter at equilibrium but, since chemical reactions may be slow, the perturbations with respect to the unstressed configuration are modeled by using a different adiabatic index. We quantify the impact of a departure of the adiabatic index from its equilibrium value on the stressed stellar configuration and we find that a small perturbation can cause large variations both in displacements and strains. As a first practical application, we estimate the strain developed between two large glitches in the Vela pulsar showing that, starting from an initial unstressed configuration, it is not possible to reach the breaking threshold of the crust, namely to trigger a starquake. In this sense, the hypothesis that starquakes could trigger the unpinning of superfluid vortices is challenged and, for the quake to be a possible trigger, the solid crust must never fully relax after a glitch, making the sequence of starquakes in a neutron star an history-dependent process.

scholarly journals Turbulent, pinned superfluids in neutron stars and pulsar glitch recoveries

2020 ◽  
Vol 499 (1) ◽  
pp. 161-170
Author(s):  
B Haskell ◽  
D Antonopoulou ◽  
C Barenghi
Keyword(s):  
Neutron Star ◽  
Second Derivative ◽  
Mutual Friction ◽  
Turbulent Model ◽  
Turbulent Region ◽  
Rotational Evolution ◽  
Vela Pulsar ◽  
Superfluid Vortices ◽  
Insight Into ◽  
Better Than

ABSTRACT Pulsar glitches offer an insight into the dynamics of superfluids in the high-density interior of a neutron star. To model these phenomena, however, one needs to have an understanding of the dynamics of a turbulent array of superfluid vortices moving through a pinning lattice. In this paper, we develop a theoretical approach to describe vortex-mediated mutual friction in a pinned, turbulent and rotating superfluid. Our model is then applied to the study of the post-glitch rotational evolution in the Vela pulsar and in PSR J0537-6910. We show that in both cases a turbulent model fits the evolution of the spin frequency derivative better than a laminar one. We also predict that the second derivative of the frequency after a glitch should be correlated with the waiting time since the previous glitch, which we find to be consistent with observational data for these pulsars. The main conclusion of this paper is that in the post-glitch rotational evolution of these two pulsars we are most likely observing the response to the glitch of a pinned turbulent region of the star (possibly the crust) and not the laminar response of a regular straight vortex array.

scholarly journals A Rocket Model of Neutrino Jet for Pulsar Kicks

2004 ◽  
Vol 218 ◽  
pp. 33-36
Author(s):  
Q. H. Peng ◽  
L. D. Zhang ◽  
X. L. Luo ◽  
C. K. Chou
Keyword(s):  
Neutron Star ◽  
Neutrino Emission ◽  
Superfluid Vortices

On the basis of the neutrino emission from the isotropic 1S0 neutron superfluid vortices in neutron star interiors, we propose a rocket model of neutrino jet for the observed pulsar kick.

Pulsar Spin Evolution, Kinematics, and the Birthrate of Neutron Star Binaries

1999 ◽  
Vol 520 (2) ◽  
pp. 696-705 ◽  
Author(s):  
Z. Arzoumanian ◽  
J. M. Cordes ◽  
I. Wasserman
Keyword(s):  
Neutron Star ◽  
Spin Evolution

scholarly journals Aperiodic Flux Variability in A 0535+262

1996 ◽  
Vol 165 ◽  
pp. 313-319
Author(s):  
Mark H. Finger ◽  
Robert B. Wilson ◽  
B. Alan Harmon ◽  
William S. Paciesas
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Beat Frequency ◽  
Power Spectra ◽  
Center Frequency ◽  
X Ray ◽  
Binary Pulsar ◽  
Transient Source ◽  
Flux Variability ◽  
Burst And Transient Source

A “giant” outburst of A 0535+262, a transient X-ray binary pulsar, was observed in 1994 February and March with the Burst and Transient Source Experiment (BATSE) onboard the Compton Gamma-Ray Observatory. During the outburst power spectra of the hard X-ray flux contained a QPO-like component with a FWHM of approximately 50% of its center frequency. Over the course of the outburst the center frequency rose smoothly from 35 mHz to 70 mHz and then fell to below 40 mHz. We compare this QPO frequency with the neutron star spin-up rate, and discuss the observed correlation in terms of the beat frequency and Keplerian frequency QPO models in conjunction with the Ghosh-Lamb accretion torque model.

A nearby neutron-star merger explains the actinide abundances in the early Solar System

Nature ◽  
2019 ◽  
Vol 569 (7754) ◽  
pp. 85-88 ◽  
Author(s):  
Imre Bartos ◽  
Szabolcs Marka
Keyword(s):  
Neutron Star ◽  
Solar System ◽  
Early Solar System

scholarly journals Multiple Pulsar Ejection in Supernova Events

1971 ◽  
Vol 46 ◽  
pp. 378-381
Author(s):  
F. Curtis Michel
Keyword(s):  
Star Formation ◽  
Neutron Star ◽  
Energy Loss

Fragmentation in the collapse of a supernova core, followed by energy loss in neutron star formation, is shown to lead to disruption of the resulting system. The elements of the system, some of which should be pulsars, can attain velocities of the order of 103 km/sec if currently quoted parameters are correct.

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