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 NGC 300 ULX1: A test case for accretion torque theory

2018 ◽  
Vol 620 ◽  
pp. L12 ◽  
Author(s):  
G. Vasilopoulos ◽  
F. Haberl ◽  
S. Carpano ◽  
C. Maitra
Keyword(s):  
Neutron Star ◽  
Test Case ◽  
X Ray ◽  
Spin Period ◽  
Spin Evolution ◽  
Spin Reversal ◽  
Eddington Limit

NGC 300 ULX1 is a newly identified ultra-luminous X-ray pulsar. The system is associated with the supernova impostor SN 2010da that was later classified as a possible supergiant Be X-ray binary. In this work we report on the spin period evolution of the neutron star based on all the currently available X-ray observations of the system. We argue that the X-ray luminosity of the system has remained almost constant since 2010, at a level above ten times the Eddington limit. Moreover, we find evidence that the spin period of the neutron star evolved from ∼126 s down to ∼18 s within a period of about 4 years. We explain this unprecedented spin evolution in terms of the standard accretion torque theory. An intriguing consequence for NGC 300 ULX1 is that a neutron star spin reversal should have occurred a few years after the SN 2010da event.

scholarly journals Discovery of a retrogradely rotating neutron star in the X-ray pulsar GX 301–2

2020 ◽  
Vol 494 (2) ◽  
pp. 2178-2182
Author(s):  
Juhani Mönkkönen ◽  
Victor Doroshenko ◽  
Sergey S Tsygankov ◽  
Armin Nabizadeh ◽  
Pavel Abolmasov ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Orbital Motion ◽  
X Ray ◽  
Spin Evolution ◽  
Ultimate Result ◽  
Term Monitoring ◽  
Direction Opposite ◽  
Principal Possibility

ABSTRACT We report on the analysis of the spin evolution of a slow X-ray pulsar GX 301–2 along the orbit using long-term monitoring by Fermi/Gamma-ray Burst Monitor. Based on the observationally confirmed accretion scenario and an analytical model for the accretion of angular momentum, we demonstrate that in this system, the neutron star spins retrogradely, that is, in a direction opposite to the orbital motion. This first-of-a-kind discovery of such a system proves the principal possibility of retrograde rotation in accreting systems with suitable accretion torque, and might have profound consequences for our understanding of the spin evolution of X-ray pulsars, estimates of their initial spin periods, and the ultimate result of their evolution.

scholarly journals Spin evolution of a proto-neutron star

2016 ◽  
Vol 94 (2) ◽  
Author(s):  
Giovanni Camelio ◽  
Leonardo Gualtieri ◽  
José A. Pons ◽  
Valeria Ferrari
Keyword(s):  
Neutron Star ◽  
Spin Evolution ◽  
Proto Neutron Star

scholarly journals Spin evolution of neutron stars in wind-fed high-mass X-ray binaries

2020 ◽  
Vol 72 (6) ◽  
Author(s):  
Shigeyuki Karino
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Neutron Stars ◽  
Wind Velocity ◽  
High Mass ◽  
Quasi Equilibrium ◽  
Pulse Period ◽  
X Ray ◽  
Spin Evolution ◽  
The Magnetic Field

Abstract The observed X-ray pulse period of OB-type high-mass X-ray binary (HMXB) pulsars is typically longer than 100 seconds. It is considered that the interaction between the strong magnetic field of a neutron star and the wind matter could cause such a long pulse period. In this study, we follow the spin evolution of neutron stars, taking into account the interaction between the magnetic field and wind matter. In this line, as new challenges, we solve the evolution of the magnetic field of the neutron star at the same time, and additionally we focus on the effects of the wind properties of the donor. As a result, evolutionary tracks were obtained in which the neutron star spends some duration in the ejector phase after birth, then rapidly spins down, becomes quasi-equilibrium, and gradually spins up. Such evolution is similar to previous studies, but we found that its dominant physics depends on the velocity of the donor wind. When the wind velocity is fast, the spin-down occurs due to magnetic inhibition, while the classical propeller effect and settling accretion shell causes rapid spin-down in the slow wind accretion. Since the wind velocity of the donor could depend on the irradiated X-ray luminosity, the spin evolution track of the neutron star in a wind-fed HMXB could be more complicated than considered.

Neutron star spin evolution: A semi-analytical approach

2000 ◽  
Author(s):  
Antonino La Barbera
Keyword(s):  
Neutron Star ◽  
Analytical Approach ◽  
Spin Evolution

Superfluid state for Galaxy's youngest neutron star?

Nature ◽  
2011 ◽  
Author(s):  
Kate McAlpine
Keyword(s):  
Neutron Star ◽  
Superfluid State

Radiation-dominated boundary layer between accretion disc and neutron star surface: theory and observations

2014 ◽  
Vol 184 (4) ◽  
pp. 409-422
Author(s):  
Marat R. Gil'fanov ◽  
Rashid A. Syunyaev
Keyword(s):  
Boundary Layer ◽  
Neutron Star ◽  
Accretion Disc ◽  
Surface Theory ◽  
Star Surface
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