Relativistic periastron shift and orbital period in a star–black-hole binary system

1997 ◽  
Vol 55 (4) ◽  
pp. 1783-1787 ◽  
Author(s):  
E. P. Esteban ◽  
F. Díaz
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Orbital Period ◽  
Black Hole Binary

VLBI OBSERVATIONS OF THE SHORTEST ORBITAL PERIOD BLACK HOLE X-RAY BINARY

2012 ◽  
Vol 08 ◽  
pp. 380-383
Author(s):  
ZSOLT PARAGI ◽  
TOMASO M. BELLONI ◽  
ALEXANDER J. VAN DER HORST ◽  
JAMES MILLER-JONES
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Orbital Period ◽  
X Ray ◽  
Show Evidence ◽  
Multi Wavelength ◽  
Black Hole Binary ◽  
Wavelength Monitoring ◽  
Early Phases ◽  
Extended Emission

The X-ray transient MAXI J1659-152 was discovered by Swift/BAT and it was initially identified as a GRB. Soon its Galactic origin and binary nature were established. There exists a wealth of multi-wavelength monitoring data for this source, providing a great coverage of the full X-ray transition in this candidate black hole binary system. We obtained two epochs of EVN/e-VLBI and four epochs of VLBA data of MAXI J1659-152 which show evidence for some extended emission in the early phases but –against expectations– no major collimated ejecta during the accretion disk state transition. This might be related to the fact that, with a red dwarf donor star, MAXI J1659-152 is the shortest orbital period black hole X-ray binary system.

scholarly journals A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102?

2015 ◽  
Vol 452 (3) ◽  
pp. 2540-2545 ◽  
Author(s):  
D. J. D'Orazio ◽  
Z. Haiman ◽  
P. Duffell ◽  
B. D. Farris ◽  
A. I. MacFadyen
Keyword(s):  
Black Hole ◽  
Orbital Period ◽  
Supermassive Black Hole ◽  
Black Hole Binary

scholarly journals Prospects for the Discovery of Black Hole Binaries without Mass Accretion with Gaia

2016 ◽  
Vol 12 (S324) ◽  
pp. 41-42
Author(s):  
Norita Kawanaka ◽  
Masaki Yamaguchi ◽  
Tsvi Piran ◽  
Tomasz Bulik
Keyword(s):  
Mass Transfer ◽  
Black Holes ◽  
Black Hole ◽  
Orbital Period ◽  
Proper Motion ◽  
Binary Systems ◽  
Evolution Model ◽  
Black Hole Binaries ◽  
Black Hole Binary ◽  
Binary Evolution

AbstractWe study the prospect for Gaia to detect black hole binary systems without the mass transfer from their companion stars. Gaia will be able to discover Galactic black holes without mass accretion by detecting the proper motion of their companion stars. We evaluate the number of such black hole binaries which have the orbital period short enough to be detected by Gaia during its operation, taking into account the binary evolution model.

High lithium abundance in the secondary of the black-hole binary system V404 Cygni

Nature ◽  
1992 ◽  
Vol 358 (6382) ◽  
pp. 129-131 ◽  
Author(s):  
E. L. Martín ◽  
R. Rebolo ◽  
J. Casares ◽  
P. A. Charles
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Lithium Abundance ◽  
Black Hole Binary

Improved Parameters for the Black Hole Binary System X-Ray Nova MUSCAE 1991

1996 ◽  
Vol 468 ◽  
pp. 380 ◽  
Author(s):  
Jerome A. Orosz ◽  
Charles D. Bailyn ◽  
Jeffrey E. McClintock ◽  
Ronald A. Remillard
Keyword(s):  
Black Hole ◽  
Binary System ◽  
X Ray ◽  
Black Hole Binary

scholarly journals VLBI observations of the shortest orbital period black hole binary, MAXI J1659−152

2013 ◽  
Vol 432 (2) ◽  
pp. 1319-1329 ◽  
Author(s):  
Z. Paragi ◽  
A. J. van der Horst ◽  
T. Belloni ◽  
J. C. A. Miller-Jones ◽  
J. Linford ◽  
...  
Keyword(s):  
Black Hole ◽  
Orbital Period ◽  
Vlbi Observations ◽  
Black Hole Binary

scholarly journals A noninteracting low-mass black hole–giant star binary system

Science ◽  
2019 ◽  
Vol 366 (6465) ◽  
pp. 637-640 ◽  
Author(s):  
Todd A. Thompson ◽  
Christopher S. Kochanek ◽  
Krzysztof Z. Stanek ◽  
Carles Badenes ◽  
Richard S. Post ◽  
...  
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Orbital Period ◽  
Binary Systems ◽  
Photometric Variability ◽  
Giant Star ◽  
Massive Neutron Star ◽  
The Galaxy ◽  
Low Mass ◽  
Star Binary

Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near-zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant’s mass and radius imply that the unseen companion is 3.3−0.7+2.8 solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.

scholarly journals The X-Ray Outburst of PG 1553+113: A Precession Effect of Two Jets in the Supermassive Black Hole Binary System

2021 ◽  
Vol 922 (2) ◽  
pp. 222
Author(s):  
Shifeng Huang ◽  
Hongxing Yin ◽  
Shaoming Hu ◽  
Xu Chen ◽  
Yunguo Jiang ◽  
...  
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Light Curve ◽  
Quiescent State ◽  
Black Hole Mass ◽  
X Ray ◽  
Supermassive Black Hole ◽  
System A ◽  
Black Hole Binary ◽  
Two Jets

Abstract Blazar PG 1553+113 is thought to be a host of supermassive black hole binary system. A 2.2 yr quasi-periodicity in the γ-ray light curve was detected, possibly a result of jet precession. Motivated by the previous studies based on the γ-ray data, we analyzed the X-ray light curve and spectra observed during 2012–2020. The 2.2 yr quasi-periodicity might be consistent with the main-flare recurrence in the X-ray light curve. When a weak rebrightening in the γ-ray was observed, a corresponding relatively strong brightening in the X-ray light curve can be identified. The harder-when-brighter tendency in both X-ray main and weak flares was shown, as well as a weak softer-when-brighter behavior for the quiescent state. We explore the possibility that the variability in the X-ray band can be interpreted with two-jet precession scenario. Using the relation between jets and accretion disks, we derive the primary black hole mass ≃3.47 × 108 M ☉ and mass of the secondary one ≃1.40 × 108 M ☉, and their mass ratio ∼0.41.

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