The Probability Distribution of Binary Pulsar Coalescence Rates. I. Double Neutron Star Systems in the Galactic Field

2003 ◽  
Vol 584 (2) ◽  
pp. 985-995 ◽  
Author(s):  
C. Kim ◽  
V. Kalogera ◽  
D. R. Lorimer
Keyword(s):  
Neutron Star ◽  
Probability Distribution ◽  
Binary Pulsar ◽  
Galactic Field

scholarly journals Binary pulsar evolution: unveiled links and new species

2012 ◽  
Vol 8 (S291) ◽  
pp. 121-126
Author(s):  
Andrea Possenti
Keyword(s):  
New Species ◽  
Neutron Star ◽  
Evolutionary Path ◽  
Binary Pulsar ◽  
Galactic Field ◽  
New Class ◽  
Binary Pulsars ◽  
Low Mass ◽  
Pulsar Searches ◽  
Pulsar Evolution

AbstractIn the last years a series of blind and/or targeted pulsar searches led to almost triple the number of known binary pulsars in the galactic field with respect to a decade ago. The focus will be on few outliers, which are emerging from the average properties of the enlarged binary pulsar population. Some of them may represent the long sought missing links between two kinds of neutron star binaries, while others could represent the stereotype of new groups of binaries, resulting from an evolutionary path which is more exotic than those considered until recently. In particular, a new class of binaries, which can be dubbed Ultra Low Mass Binary Pulsars (ULMBPs), is emerging from recent data.

scholarly journals The Probability Distribution Of Binary Pulsar Coalescence Rates. II. Neutron Star–White Dwarf Binaries

2004 ◽  
Vol 616 (2) ◽  
pp. 1109-1117 ◽  
Author(s):  
Chunglee Kim ◽  
Vassiliki Kalogera ◽  
Duncan R. Lorimer ◽  
Tiffany White
Keyword(s):  
Neutron Star ◽  
Probability Distribution ◽  
White Dwarf ◽  
Binary Pulsar

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.

scholarly journals Anisotropic neutron stars by gravitational decoupling

2019 ◽  
Vol 79 (10) ◽  
Author(s):  
V. A. Torres-Sánchez ◽  
E. Contreras
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Perfect Fluid ◽  
Compact Object ◽  
Adiabatic Index ◽  
X Ray ◽  
Binary Pulsar ◽  
Stable Solutions ◽  
X Ray Binaries ◽  
Fluid Configuration

Abstract In this work we obtain an anisotropic neutron star solution by gravitational decoupling starting from a perfect fluid configuration which has been used to model the compact object PSR J0348+0432. Additionally, we consider the same solution to model the Binary Pulsar SAX J1808.4-3658 and X-ray Binaries Her X-1 and Cen X-3 ones. We study the acceptability conditions and obtain that the MGD-deformed solution obey the same physical requirements as its isotropic counterpart. Finally, we conclude that the most stable solutions, according to the adiabatic index and gravitational cracking criterion, are those with the smallest compactness parameters, namely SAX J1808.4-3658 and Her X-1.

scholarly journals Shall we Observe a Radio Binary Pulsar in SN 1987A?

1992 ◽  
Vol 128 ◽  
pp. 222-224
Author(s):  
Qiao G. J.
Keyword(s):  
Neutron Star ◽  
Surface Temperature ◽  
High Surface ◽  
Star Model ◽  
Single Star ◽  
X Ray ◽  
Binary Pulsar ◽  
Collapse Model ◽  
High Surface Temperature ◽  
Γ Ray

AbstractAn induced-collapse model [hereafter IC model; He et al. (1990)] can overcome the problems of the single star model of SN1987A. According to the IC model, there is a possibility that the SN1987A remnant will be a binary system with two neutron stars, one of them (SK-69 202) will have a strong magnetic field and a high surface temperature which favors detection as an X-ray or γ-ray pulsar. If the surface temperature of the neutron star cools down to T = 107 K, a radio binary pulsar is expected. There is also the possibility that an X-ray or γ-ray pulsar will be observed first, and only later will a radio pulsar will be detected.A newly formed neutron star is thought to have a short (millisecond) period. In this case, the core emission beam is then very large (Qiao 1992) and is thus very likely to swing in the direction of the Earth.

scholarly journals RX J0529.8−6556: a BeXRB pulsar with an evolving optical period and out of phase X-ray outbursts

2021 ◽  
Vol 503 (4) ◽  
pp. 6187-6201
Author(s):  
H Treiber ◽  
G Vasilopoulos ◽  
C D Bailyn ◽  
F Haberl ◽  
K C Gendreau ◽  
...  
Keyword(s):  
Neutron Star ◽  
Orbital Period ◽  
Orbital Plane ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Optical Data ◽  
Pulse Profile ◽  
X Ray ◽  
Binary Pulsar ◽  
Be Star

ABSTRACT We report the results of eROSITA and NICER observations of the 2020 June outburst of the Be/X-ray binary pulsar RX J0529.8−6556 in the Large Magellanic Cloud, along with the analysis of archival X-ray and optical data from this source. We find two anomalous features in the system’s behaviour. First, the pulse profile observed by NICER during maximum luminosity is similar to that observed by XMM–Newton in 2000, despite the fact that the X-ray luminosity was different by two orders of magnitude. In contrast, a modest decrease in luminosity in the 2020 observations generated a significant change in pulse profile. Secondly, we find that the historical optical outbursts are not strictly periodic, as would be expected if the outbursts were triggered by periastron passage, as is generally assumed. The optical peaks are also not coincident with the X-ray outbursts. We suggest that this behaviour may result from a misalignment of the Be star disc and the orbital plane, which might cause changes in the timing of the passage of the neutron star through the disc as it precesses. We conclude that the orbital period of the source remains unclear.

scholarly journals The Green Bank Northern Celestial Cap Pulsar Survey. VI. Discovery and Timing of PSR J1759+5036: A Double Neutron Star Binary Pulsar

2021 ◽  
Vol 922 (1) ◽  
pp. 35
Author(s):  
G. Y. Agazie ◽  
M. G. Mingyar ◽  
M. A. McLaughlin ◽  
J. K. Swiggum ◽  
D. L. Kaplan ◽  
...  
Keyword(s):  
Neutron Star ◽  
Major Axis ◽  
Total System ◽  
Semi Major Axis ◽  
Binary Pulsar ◽  
Orbital Parameters ◽  
Spin Period ◽  
Timing Data ◽  
Star Binary ◽  
Radio Transients

Abstract The Green Bank North Celestial Cap survey is a 350 MHz all-sky survey for pulsars and fast radio transients using the Robert C. Byrd Green Bank Telescope. To date, the survey has discovered over 190 pulsars, including 33 millisecond pulsars and 24 rotating radio transients. Several exotic pulsars have been discovered in the survey, including PSR J1759+5036, a binary pulsar with a 176 ms spin period in an orbit with a period of 2.04 days, an eccentricity of 0.3, and a projected semi-major axis of 6.8 light seconds. Using seven years of timing data, we are able to measure one post–Keplerian parameter, advance of periastron, which has allowed us to constrain the total system mass to 2.62 ± 0.03 M ⊙. This constraint, along with the spin period and orbital parameters, suggests that this is a double neutron star system, although we cannot entirely rule out a pulsar-white dwarf binary. This pulsar is only detectable in roughly 45% of observations, most likely due to scintillation. However, additional observations are required to determine whether there may be other contributing effects.

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