scholarly journals Long-term evolution of a merger-remnant neutron star in general relativistic magnetohydrodynamics: Effect of magnetic winding

2021 ◽  
Vol 103 (4) ◽  
Author(s):  
Masaru Shibata ◽  
Sho Fujibayashi ◽  
Yuichiro Sekiguchi
Keyword(s):  
Neutron Star ◽  
Long Term Evolution ◽  
Term Evolution ◽  
General Relativistic ◽  
Relativistic Magnetohydrodynamics

scholarly journals The long-term evolution of neutron star merger remnants - I. The impact of r-process nucleosynthesis

2014 ◽  
Vol 439 (1) ◽  
pp. 744-756 ◽  
Author(s):  
S. Rosswog ◽  
O. Korobkin ◽  
A. Arcones ◽  
F.- K. Thielemann ◽  
T. Piran
Keyword(s):  
Neutron Star ◽  
Long Term Evolution ◽  
Term Evolution ◽  
R Process ◽  
The Impact

Long-term evolution of crustal neutron star magnetic fields

1994 ◽  
Vol 433 ◽  
pp. 780 ◽  
Author(s):  
V. A. Urpin ◽  
G. Chanmugam ◽  
Yeming Sang
Keyword(s):  
Neutron Star ◽  
Magnetic Fields ◽  
Long Term Evolution ◽  
Term Evolution

scholarly journals Long-term evolution of CFS-unstable neutron stars and the role of differential rotation on short time-scales

2018 ◽  
Vol 482 (3) ◽  
pp. 3045-3057 ◽  
Author(s):  
A I Chugunov
Keyword(s):  
Neutron Star ◽  
Time Scales ◽  
Differential Rotation ◽  
Time Scale ◽  
Evolution Equations ◽  
Long Term Evolution ◽  
Cooling Power ◽  
Term Evolution ◽  
Short Time

Abstract I consider differential rotation, associated with radiation-driven Chandrasekhar–Friedman–Schutz (CFS) instability, and respective observational manifestations. I focus on the evolution of the apparent spin frequency, which is typically associated with the motion of a specific point on the stellar surface (e.g. polar cap). I start from long-term evolution (on the time-scale when instability significantly changes the spin frequency). For this case, I reduce the evolution equations to one differential equation and I demonstrate that it can be directly derived from energy conservation law. This equation governs the evolution rate through a sequence of thermally equilibrium states and it provides linear coupling for the cooling power and rotation energy losses via gravitational wave emission. In particular, it shows that differential rotation does not affect long-term spin-down. In contrast, on short time-scales, differential rotation can significantly modify the apparent spin-down, if we examine a strongly unstable star with a very small initial amplitude for the unstable mode. This statement is confirmed by considering a Newtonian non-magnetized perfect fluid and dissipative stellar models as well as a magnetized stellar model. For example, despite the fact that the widely applied evolution equations predict effective spin to be constant in the absence of dissipation, the CFS-unstable star should be observed as spinning-down. However, the effects of differential rotation on apparent spin-down are negligible for realistic models of neutron star recycling, unless the neutron star is non-magnetized, the r-mode amplitude is modulated faster than the shear viscosity dissipation time-scale, and the amplitude is large enough that spin-down can be measured on a modulation time-scale.

scholarly journals Long-term evolution of the neutron-star spin period of SXP 1062

2013 ◽  
Vol 556 ◽  
pp. A139 ◽  
Author(s):  
R. Sturm ◽  
F. Haberl ◽  
L. M. Oskinova ◽  
M. P. E. Schurch ◽  
V. Hénault-Brunet ◽  
...  
Keyword(s):  
Neutron Star ◽  
Long Term Evolution ◽  
Spin Period ◽  
Term Evolution

scholarly journals The long-term evolution of neutron star merger remnants – II. Radioactively powered transients

2014 ◽  
Vol 439 (1) ◽  
pp. 757-770 ◽  
Author(s):  
Doron Grossman ◽  
Oleg Korobkin ◽  
Stephan Rosswog ◽  
Tsvi Piran
Keyword(s):  
Neutron Star ◽  
Long Term Evolution ◽  
Term Evolution
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