Evolution of High-mass X-ray binaries in the Small Magellanic Cloud

2018 ◽  
Vol 14 (S346) ◽  
pp. 353-357
Author(s):  
Jun Yang ◽  
Daniel R. Wik
Keyword(s):  
Neutron Star ◽  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
Third Body ◽  
X Ray ◽  
Spin Period ◽  
Period Derivative ◽  
X Ray Binaries ◽  
Small Period

AbstractIn order to understand the progenitor of rotation powered pulsars, we compare them with High-mass X-ray binary (HMXB) pulsars, (or X-ray pulsars), in the Small Magellanic Cloud. The plot of period period vs. period derivative shows that isolated neutron stars could be evolved from HMXBs. The pulsars with long spin period might spin up to 0.001-1 s. The mechanism is a third-body interaction that detaches the donor, leaving an isolated, small period neutron star behind.

scholarly journals Early neutron star evolution in high-mass X-ray binaries

2020 ◽  
Vol 494 (1) ◽  
pp. 44-49 ◽  
Author(s):  
Wynn C G Ho ◽  
M J P Wijngaarden ◽  
Nils Andersson ◽  
Thomas M Tauris ◽  
F Haberl
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Thermal Emission ◽  
Equilibrium Phase ◽  
High Mass ◽  
X Ray ◽  
Spin Period ◽  
Long Duration ◽  
X Ray Binaries ◽  
The Magnetic Field

ABSTRACT The application of standard accretion theory to observations of X-ray binaries provides valuable insights into neutron star (NS) properties, such as their spin period and magnetic field. However, most studies concentrate on relatively old systems, where the NS is in its late propeller, accretor, or nearly spin equilibrium phase. Here, we use an analytic model from standard accretion theory to illustrate the evolution of high-mass X-ray binaries (HMXBs) early in their life. We show that a young NS is unlikely to be an accretor because of the long duration of ejector and propeller phases. We apply the model to the recently discovered ∼4000 yr old HMXB XMMU J051342.6−672412 and find that the system’s NS, with a tentative spin period of 4.4 s, cannot be in the accretor phase and has a magnetic field B > a few × 1013 G, which is comparable to the magnetic field of many older HMXBs and is much higher than the spin equilibrium inferred value of a few × 1011 G. The observed X-ray luminosity could be the result of thermal emission from a young cooling magnetic NS or a small amount of accretion that can occur in the propeller phase.

scholarly journals On the geometry of the X-ray emission from pulsars: the changing aspect of the Be/X-ray pulsar SXP348

2019 ◽  
Vol 486 (3) ◽  
pp. 3248-3258
Author(s):  
R Cappallo ◽  
S G T Laycock ◽  
D M Christodoulou ◽  
M J Coe ◽  
A Zezas
Keyword(s):  
Binary System ◽  
Point Source ◽  
Geometric Model ◽  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Spin Period ◽  
The Past ◽  
Model Fits

ABSTRACT The X-ray source SXP348 is a high-mass X-ray binary system in the Small Magellanic Cloud. Since its 1998 discovery by BeppoSAX, this pulsar has exhibited a spin period of ∼340−350 s. In an effort to determine the orientation and magnetic geometry of this source, we used our geometric model Polestar to fit 71 separate pulse profiles extracted from archival Chandra and XMM-Newton observations over the past two decades. During 2002, pulsations ceased being detectable for nine months despite the source remaining in a bright state. When pulsations resumed, our model fits changed, displaying a change in accretion geometry. Furthermore, in 2006, detectable pulsations again ceased, with 2011 marking the last positive detection of SXP348 as a point source. These profile fits will be released for public use as part of the database of Magellanic Cloud pulsars.

scholarly journals Orbital and superorbital periods in ULX pulsars, disc-fed HMXBs, Be/X-ray binaries, and double-periodic variables

2020 ◽  
Vol 495 (1) ◽  
pp. L139-L143
Author(s):  
L J Townsend ◽  
P A Charles
Keyword(s):  
Neutron Star ◽  
Orbital Period ◽  
Binary Systems ◽  
High Mass ◽  
Early Type ◽  
Present Evidence ◽  
X Ray ◽  
Spin Period ◽  
Simple Linear Relationship ◽  
X Ray Binaries

ABSTRACT We present evidence for a simple linear relationship between the orbital period and superorbital period in ultra-luminous X-ray (ULX) pulsars, akin to what is seen in the population of disc-fed neutron star supergiant X-ray binary and Be/X-ray binary systems. We argue that the most likely cause of this relationship is the modulation of precessing hotspots or density waves in an accretion or circumstellar disc by the binary motion of the system, implying a physical link between ULX pulsars and high-mass X-ray binary (HMXB) pulsars. This hypothesis is supported by recent studies of Galactic and Magellanic Cloud HMXBs accreting at super-Eddington rates, and the position of ULX pulsars on the spin period–orbital period diagram of HMXBs. An interesting secondary relationship discovered in this work is the apparent connection between disc-fed HMXBs, ULXs, and a seemingly unrelated group of early-type binaries showing so-called double-periodic variability. We suggest that these systems are good candidates to be the direct progenitors of Be/X-ray binaries.

scholarly journals The superslow pulsation X-ray pulsars in high mass X-ray binaries

2012 ◽  
Vol 8 (S291) ◽  
pp. 203-206 ◽  
Author(s):  
Wei Wang
Keyword(s):  
Neutron Star ◽  
Binary Systems ◽  
High Mass ◽  
X Ray ◽  
Origin And Evolution ◽  
Surface Magnetic Field ◽  
Spin Period ◽  
Binary Evolution ◽  
X Ray Binaries

AbstractThere exists a special class of X-ray pulsars that exhibit very slow pulsation of Pspin > 1000 s in the high mass X-ray binaries (HMXBs). We have studied the temporal and spectral properties of these superslow pulsation neutron star binaries in hard X-ray bands with INTEGRAL observations. Long-term monitoring observations find spin period evolution of two sources: spin-down trend for 4U 2206+54 (Pspin ~ 5560 s with Ṗspin ~ 4.9 × 10−7 s s−1) and long-term spin-up trend for 2S 0114+65 (Pspin ~ 9600 s with Ṗspin ~ −1 × 10−6 s s−1) in the last 20 years. A Be X-ray transient, SXP 1062 (Pspin ~ 1062 s), also showed a fast spin-down rate of Ṗspin ~ 3 × 10−6 s s−1 during an outburst. These superslow pulsation neutron stars cannot be produced in the standard X-ray binary evolution model unless the neutron star has a much stronger surface magnetic field (B > 1014 G). The physical origin of the superslow spin period is still unclear. The possible origin and evolution channels of the superslow pulsation X-ray pulsars are discussed. Superslow pulsation X-ray pulsars could be younger X-ray binary systems, still in the fast evolution phase preceding the final equilibrium state. Alternatively, they could be a new class of neutron star system – accreting magnetars.

Evolution of high-mass X-ray binaries in the small magellanic cloud

2019 ◽  
Vol 340 (1-3) ◽  
pp. 46-49
Author(s):  
J. Yang ◽  
D. R. Wik ◽  
A. Zezas ◽  
S. G. T. Laycock ◽  
J. Hong ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
X Ray Binaries

scholarly journals Deep Chandra Survey of the Small Magellanic Cloud. III. Formation Efficiency of High-mass X-Ray Binaries

2019 ◽  
Vol 887 (1) ◽  
pp. 20 ◽  
Author(s):  
Vallia Antoniou ◽  
Andreas Zezas ◽  
Jeremy J. Drake ◽  
Carles Badenes ◽  
Frank Haberl ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Formation Efficiency ◽  
X Ray Binaries

scholarly journals The slow X-ray pulsar SXP 1062 and associated supernova remnant in the Wing of the Small Magellanic Cloud

2012 ◽  
Vol 8 (S291) ◽  
pp. 459-461 ◽  
Author(s):  
L. M. Oskinova ◽  
M. A. Guerrero ◽  
V. Hénault-Brunet ◽  
W. Sun ◽  
Y.-H. Chu ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Theoretical Models ◽  
Exceptional Case ◽  
High Mass ◽  
Unique Combination ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Spin Period ◽  
Star Evolution

AbstractSXP 1062 is an exceptional case of a young neutron star in a wind-fed high-mass X-ray binary associated with a supernova remnant. A unique combination of measured spin period, its derivative, luminosity and young age makes this source a key probe for the physics of accretion and neutron star evolution. Theoretical models proposed to explain the properties of SXP 1062 shall be tested with new data.

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