scholarly journals Close Binaries with Two Compact Objects

2000 ◽  
Vol 177 ◽  
pp. 579-584
Author(s):  
V. Kalogera
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
Binary Systems ◽  
Compact Objects ◽  
Close Binary ◽  
Close Binaries ◽  
Upper Limit ◽  
Coalescence Rate ◽  
Laser Interferometers

AbstractThe coalescence of close binary systems with two compact objects (neutron stars and black holes) are considered to be promising sources of gravitational waves for the currently built laser interferometers. Here, I review the current Galactic coalescence estimates derived both theoretically and empirically. I discuss the uncertainties involved as well as ways of obtaining an upper limit to the coalescence rate of two neutron stars.

scholarly journals Accretion onto Relativistic Objects

1974 ◽  
Vol 64 ◽  
pp. 194-212
Author(s):  
M. J. Rees
Keyword(s):  
Black Holes ◽  
Interstellar Medium ◽  
Neutron Stars ◽  
Binary Systems ◽  
Compact Object ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Compact Objects ◽  
X Ray ◽  
Intergalactic Space

The physics of spherically symmetrical accretion onto a compact object is briefly reviewed. Neither neutron stars nor stellar-mass black holes are likely to be readily detectable if they are isolated and accreting from the interstellar medium. Supermassive black holes in intergalactic space may however be detectable. The effects of accretion onto compact objects in binary systems are then discussed, with reference to the phenomena observed in variable X-ray sources.

scholarly journals Late Stages of the Evolution of Close Binaries

1984 ◽  
Vol 80 ◽  
pp. 335-354
Author(s):  
C. De Loore ◽  
W. Sutantyo
Keyword(s):  
Mass Transfer ◽  
Neutron Stars ◽  
Binary Systems ◽  
Exceptional Case ◽  
Compact Objects ◽  
Close Binaries ◽  
Millisecond Pulsar ◽  
X Ray ◽  
Compact Component ◽  
X Ray Binaries

AbstractClose binaries can evolve through various ways of interaction into compact objects (white dwarfs, neutron stars, black holes). Massive binary systems (mass of the primary M1 larger than 14 to 15 M0) are expected to leave, after the first stage of mass transfer a compact component orbiting a massive star. These systems evolve during subsequent stages into massive X-ray binaries. Systems with initial large periode evolve into Be X-ray binaries.Low mass X-ray sources are probably descendants of lower mass stars, and various channels for their production are indicated. The evolution of massive close binaries is examined in detail and different X-ray stages are discussed. It is argued that a first X-ray stage is followed by a reverse extensive mass transfer, leading to systems like SS433, CirXl. During further evolution these systems would become Wolf-Rayet runaways. Due to spiral in these system would then further evolve into ultra short X-ray binaries like CygX-3.Finally the explosion of the secondary will in most cases disrupt the system. In an exceptional case the system remains bound, leading to binary pulsars like PSR 1913 +16. In such systems the orbit will shrink due to gravitational radiation and finally the two neutron stars will coalesce. It is argued that the millisecond pulsar PSR 1937 + 214 could be formed in this way.A complete scheme starting from two massive ZAMS stars, ending with a millisecond pulsar is presented.

scholarly journals Pulsars and Close Binary Systems

1971 ◽  
Vol 46 ◽  
pp. 273-278
Author(s):  
Virginia Trimble ◽  
Martin Rees
Keyword(s):  
Mass Transfer ◽  
Neutron Stars ◽  
Binary Systems ◽  
Alternative Explanation ◽  
Galactic Plane ◽  
Orbital Motion ◽  
Close Binary ◽  
Close Binaries ◽  
Close Binary Systems ◽  
Supernova Explosions

It is first considered what must happen if pulsars (i.e. neutron stars) are formed in close binary systems (CBS), and whether the resulting orbital motion and mass transfer should be observable. As this set of alternatives seems unlikely, there follow suggestions of how one might prevent the formation of neutron stars in close binaries. Finally, it is shown that ‘runaway’ pulsars with velocities larger than about 15 km/sec cannot be produced by isotropic supernova explosions within close binaries, and an alternative explanation is suggested for the observed correlation of periods of pulsars with their distances from the galactic plane.

scholarly journals Microquasars and ULXS: Fossils of GRB Sources

2004 ◽  
Vol 194 ◽  
pp. 14-17 ◽  
Author(s):  
I. F. Mirabell
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Binary Systems ◽  
Gamma Ray ◽  
Massive Stars ◽  
Compact Objects ◽  
Primary Star ◽  
Long Duration ◽  
Supernova Explosions ◽  
Low Mass

AbstractGamma-ray bursts (GRBs) of long duration probably result from the core-collapse of massive stars in binary systems. After the collapse of the primary star the binary system may remain bound leaving a microquasar or ULX source as remnant. In this context, microquasars and ULXs are fossils of GRB sources and should contain physical and astrophysical clues on their GRB-source progenitors. Here I show that the identification of the birth place of microquasars can provide constrains on the progenitor stars of compact objects, and that the runaway velocity can be used to constrain the energy in the explosion of massive stars that leave neutron stars and black holes. The observations show that the neutron star binaries LS 5039, LSI +61°303 and the low-mass black hole GRO J1655-40 formed in energetic supernova explosions, whereas the black holes of larger masses (M ≥ 10 M⊙) in Cygnus X-l and GRS 1915+105 formed promptly, in the dark or in underluminous supornovao. The association with clusters of massive stars of the microquasar LSI +61°303 and the magnetars SGR 1806-20 and SGR 1900+14, suggest that very massive stars (M ≥ 50 M⊙) may -in some cases- leave neutron stars rather than black holes. The models of GRB sources of long duration have the same basic ingredients as microquasars and ULXs: compact objects with accretion disks and relativistic jets in binary systems. Therefore, the analogies between microquasars and AGN may be extended to the sources of GRBs.

The XMM-NEWTON VIEW ON NEUTRON STARS AND BLACK HOLES

2004 ◽  
Vol 13 (07) ◽  
pp. 1229-1237
Author(s):  
CHRISTIAN MOTCH
Keyword(s):  
Black Holes ◽  
Spectral Analysis ◽  
Neutron Stars ◽  
Binary Systems ◽  
Short Review ◽  
High Energy ◽  
Compact Objects ◽  
High Energy Resolution ◽  
X Ray ◽  
Physical Conditions

The improved sensitivity of the XMM-Newton satellite is quickly expanding our knowledge of X-ray emission mechanisms and physical conditions in and around compact objects. Thanks to the large collecting power and high energy resolution of the EPIC and RGS instruments, detailed X-ray spectral analysis can be performed in the 0.2 to 12 keV energy range. In this short review, I highlight the most significant results obtained by XMM-Newton on neutron stars both isolated and in binary systems and on accreting stellar mass black holes.

scholarly journals Black Holes in General Relativity and Beyond

Proceedings ◽  
2019 ◽  
Vol 17 (1) ◽  
pp. 1 ◽  
Author(s):  
Enrico Barausse
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Black Hole ◽  
Gravitational Waves ◽  
Physical Interpretation ◽  
Binary Systems ◽  
Compact Objects ◽  
Black Hole Binary ◽  
Remarkable Agreement

The recent detections of gravitational waves from binary systems of black holes are in remarkable agreement with the predictions of General Relativity. In this pedagogical mini-review, I go through the physics of the different phases of the evolution of black hole binary systems, providing a qualitative physical interpretation of each one of them. I also briefly describe how these phases would be modified if gravitation were described by a theory extending or deforming General Relativity, or if the binary components turned out to be more exotic compact objects than black holes.

scholarly journals Commission 42: Close Binary Stars: (Etoiles Doubles Serrees)

2000 ◽  
Vol 24 (1) ◽  
pp. 259-276
Author(s):  
Edward F. Guinan ◽  
P. Szkody ◽  
M. Rodono ◽  
L. Bianchi ◽  
J.V. Clausen ◽  
...  
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Binary Stars ◽  
Binary Systems ◽  
Main Sequence ◽  
Magellanic Clouds ◽  
Giant Planets ◽  
Close Binary ◽  
Main Sequence Stars ◽  
Close Binary Stars

This is the last triennial report of Commission 42 for this millennium. A great deal has been accomplished in the study of Close Binary Stars (CBS) since the discovery of the first close (eclipsing) binary, Algol, in 1783 by John Goodricke. Now, over 10,000 CBS (most eclipsing variables) are known. More than 5000 of these CBS were discovered over the last several years alone! And many more are expected to be detected over the next few years. Most of these stars were found as spin-offs of microlensing surveys. Interestingly, nearly half of these stars are found outside our Galaxy, primarily in the Magellanic Clouds and M31. Every type of star is represented as a member of a close binary. These include main sequence (as well as pre-main sequence) stars, giants, and supergiants, with the entire possible range of of spectral types and masses represented. Moreover, “dying” stars and “dead” stars, such as white dwarfs, neutron stars, black holes, and, more recently, even brown dwarfs and giant planets (e.g., 51 Peg) have been found as members of close binary systems.

scholarly journals The gravitational radiation power of the blazar OJ 287

2020 ◽  
Vol 4 (4) ◽  
pp. 397-411
Author(s):  
A. E. Volvach ◽  
◽  
L. N. Volvach ◽  
M. G. Larionov ◽  
◽  
...  
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Gravitational Radiation ◽  
Binary Systems ◽  
Radiation Power ◽  
Close Binary ◽  
Frequency Monitoring ◽  
Radio Band ◽  
Harmonic Analyses ◽  
Blazar Oj 287

Using a new model based on the consideration of close binary systems (CDS) of supermassive black holes (SMBHs), we obtained data for the OJ 287 blazar, which is necessary for finding the parameters of the OJ 287 gravitational radiation. We used the results of multi-frequency monitoring performed only in the radio band. The application of harmonic analyses of observational data allowed us to construct a model of CDS consisting of two SMBHs of comparable masses, which made it possible to find the power of gravitational radiation coming from OJ 287, variations in the orbit of the double SMDS, and to consider the possibility of experimentally determining changes in these parameters in the system. Variants of radiation of electromagnetic and gravitational waves coming from OJ 287 in various states of object activity are considered.

scholarly journals Gravitational waves: A review on the future astronomy

2022 ◽  
pp. 38-50
Author(s):  
Rabinarayan Swain ◽  
Priyasmita Panda ◽  
Hena Priti Lima ◽  
Bijayalaxmi Kuanar ◽  
Biswajit Dalai
Keyword(s):  
Black Holes ◽  
Dark Matter ◽  
Dark Energy ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Binary Systems ◽  
Hubble Constant ◽  
New Approach ◽  
Different Sources

Detection of Gravitational waves opened a new path for cosmological study in a new approach. From the detection of gravitational waves signal by advanced LIGO, its research climbed the peak. After the collaboration of LIGO and Virgo, several observations get collected from different sources of binary systems like black holes, binary neutron stars even both binary black hole and neutron star. The rigorous detection of gravitational signals may provide an additional thrust in the study of complex binary systems, dark matter, dark energy, Hubble constant, etc. In this review paper, we went through multiple research manuscripts to analyze gravitational wave signals. Here we have reviewed the history and current situation of gravitational waves detection, and we explained the concept and process of detection. Also, we go through different parts of a detector and their working. Then multiple gravitational wave signals are focused, originated from various sources and then found correlation between them. From this, the contribution of gravitational waves in different fields like complex binary systems (black holes, neutron stars), dark matter, dark energy and Hubble Constant have been discussed in this manuscript.

scholarly journals Pulsar Identification of Background Spectra of LIGO Data

2018 ◽  
Vol 1 (2) ◽  
Keyword(s):  
Black Holes ◽  
Exact Solution ◽  
General Relativity ◽  
Time Delay ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Compact Objects ◽  
Gravitational Redshift ◽  
Wave Spectra

By choosing the metric (called physical metric) in general relativity as the exact solution to the Einstein equation that fits the time delay data, one can determine the size and gravitational redshift on the surface of compact objects (neutron stars and black holes). The author shows that the physical metric is invariant by rotation. As a result, the frequencies of gravitational waves from pulsars are represented as n * f / for pulsar frequency f and harmonics n. Based on this result, the author has identified potential pulsar candidates with gravitational wave spectra. This result will be critical in the study of gravitational redshift of compact objects.

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