Gravitational Force between the Black Hole and Light Particle in XRBs

AbstractA summary is given of the present state of our knowledge of High-Mass X-ray Binaries (HMXBs), their formation and expected future evolution. Among the HMXB-systems that contain neutron stars, only those that have orbital periods upwards of one year will survive the Common-Envelope (CE) evolution that follows the HMXB phase. These systems may produce close double neutron stars with eccentric orbits. The HMXBs that contain black holes do not necessarily evolve into a CE phase. Systems with relatively short orbital periods will evolve by stable Roche-lobe overflow to short-period Wolf-Rayet (WR) X-ray binaries containing a black hole. Two other ways for the formation of WR X-ray binaries with black holes are identified: CE-evolution of wide HMXBs and homogeneous evolution of very close systems. In all three cases, the final product of the WR X-ray binary will be a double black hole or a black hole neutron star binary.

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The black hole spin in coalescing binary black holes and high-mass X-ray binaries

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318007469 ◽

2018 ◽

Vol 14 (S346) ◽

pp. 426-432

Author(s):

Y. Qin ◽

T. Fragos ◽

G. Meynet ◽

P. Marchant ◽

V. Kalogera ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

High Spin ◽

High Mass ◽

Binary Black Holes ◽

X Ray ◽

Black Hole Spin ◽

Spin Properties ◽

X Ray Binaries

AbstractThe six LIGO detections of merging black holes (BHs) allowed to infer slow spin values for the two pre-merging BHs. The three cases where the spins of the BHs can be determined in high-mass X-ray binaries (HMXBs) show that those BHs have high spin values. We discuss here scenarios explaining these differences in spin properties in these two classes of object.

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Formation of Low-Mass Black Hole X-Ray Transients

Highlights of Astronomy ◽

10.1017/s153929960001875x ◽

1998 ◽

Vol 11 (2) ◽

pp. 775-778

Author(s):

Simon Portegies Zwart ◽

Frank Verbunt ◽

Ene Ergma

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

Formation Rate ◽

X Ray ◽

Low Mass ◽

X Ray Binaries

We study the formation of low-mass X-ray binaries with a black hole as accreting object. The performed semi-analytic analysis reveals that the formation rate of black holes in low-mass X-ray binaries is about two orders of magnitude smaller than that of systems with a neutron star as accretor. This is contradicted by the six observed systems, which are all transients, which suggest that the majority of these systems has not been seen jet. The birthrate for both type of objects are expected to be similar (for reviews see Cowley 1992, Tanaka & Lewin 1995).

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Observational evidence for stellar-mass black holes

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307004590 ◽

2006 ◽

Vol 2 (S238) ◽

pp. 3-12 ◽

Cited By ~ 4

Author(s):

Jorge Casares

Keyword(s):

Black Holes ◽

Black Hole ◽

Mass Spectrum ◽

Radial Velocity ◽

Stellar Mass ◽

Observational Evidence ◽

X Ray ◽

History Of ◽

X Ray Binaries ◽

Dynamical Masses

AbstractRadial velocity studies of X-ray binaries provide the most solid evidence for the existence of stellar-mass black holes. We currently have 20 confirmed cases, with dynamical masses in excess of 3 M⊙. Accurate masses have been obtained for a subset of systems which gives us a hint at the mass spectrum of the black hole population. This review summarizes the history of black hole discoveries and presents the latest results in the field.

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Be/X-Ray Binaries with Black Holes in the Galaxy and in the Magellanic Clouds

Acta Polytechnica CTU Proceedings ◽

10.14311/app.2014.01.0175 ◽

2014 ◽

Vol 1 (1) ◽

pp. 175-180 ◽

Cited By ~ 3

Author(s):

Janusz Ziolkowski

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

Magellanic Clouds ◽

X Ray ◽

The Galaxy ◽

X Ray Binaries ◽

Successful Candidate

I will start with the statistics indicating that the objects named in the title of my talk are either non-existing or very elusive to detect (not a single such object is known against 119 known Be/neutron star X-ray binaries). After brief reviewing of the properties of Be/X-ray binaries I discuss several objects that were proposed as the long sought for candidates for Be/black hole X-ray binaries. After three unsuccessful candidates (LS I +61° 303, LS 5039 and MAXI J1836-194), a successful candidate (AGL J2241+4454/MWC 656) was finally, very recently, announced.

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On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310016340 ◽

2010 ◽

Vol 6 (S275) ◽

pp. 329-330

Author(s):

Janusz Ziółkowski ◽

Krzysztof Belczyński

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

Stellar Population ◽

Magellanic Clouds ◽

Population Synthesis ◽

X Ray ◽

Stellar Population Synthesis ◽

The Galaxy ◽

X Ray Binaries

AbstractIn the Galaxy there are 67 Be X-ray binaries known to-date. Out of those, 45 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. This disparity is referred to as a missing Be – black hole X-ray binary problem. The stellar population synthesis calculations following the formation of Be X-ray binaries (Belczyński & Ziółkowski 2009) predict that the ratio of the binaries with neutron stars to the ones with black holes is rather high FNS/BH ~ 30–50. A comparison of this ratio with the number of confirmed Be – neutron star X-ray binaries (45) indicates that the expected number of Be – black hole X-ray binaries is of the order of only ~0–2. This is entirely consistent with the observed Galactic sample. Therefore, there is no problem of the missing Be+BH X-Ray Binaries for the GalaxyIn the Magellanic Clouds there are 94 Be X-ray binaries known to-date. Out of those, 60 host a neutron star. Again, none hosts a black hole. The stellar population synthesis calculations carried out specifically for the Magellanic Clouds (Ziółkowski & Belczyński 2010) predict that the ratio of the Be X-ray binaries with neutron stars to the ones with black holes is only FNS/BH ~ 10. This value is rather too low, as it implies the expected number of Be+BH X-ray binaries of the order of ~6, while none is observed. We found, that to remove the discrepancy, one has to take into account a different history of the star formation rate in the Magellanic Clouds, with the respect to the Galaxy. New stellar population synthesis calculations are currently being carried out.

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Evolution of binaries with compact objects in globular clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315007826 ◽

2014 ◽

Vol 10 (S312) ◽

pp. 203-212

Author(s):

Natalia Ivanova

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Stars ◽

Globular Clusters ◽

Compact Objects ◽

Stellar Systems ◽

Stellar Objects ◽

X Ray ◽

Low Mass ◽

X Ray Binaries

AbstractDynamical interactions that take place between objects in dense stellar systems lead to frequent formation of exotic stellar objects, unusual binaries, and systems of higher multiplicity. They are most important for the formation of binaries with neutron stars and black holes, which are usually observationally revealed in mass-transferring binaries. Here we review the current understanding of compact object's retention, of the metallicity dependence on the formation of low-mass X-ray binaries with neutron stars, and how mass-transferring binaries with a black hole and a white dwarf can be formed. We discuss as well one old unsolved puzzle and two new puzzles posed by recent observations: what descendants do ultra-compact X-ray binaries produce, how are very compact triples formed, and how can black hole low-mass X-ray binaries acquire non-degenerate companions?

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CONSTRAINTS ON X-RAY POLARIZATION OF SYNCHROTRON JETS FROM STELLAR-MASS BLACK HOLES

International Journal of Modern Physics Conference Series ◽

10.1142/s2010194512004473 ◽

2012 ◽

Vol 08 ◽

pp. 102-107

Author(s):

D. M. RUSSELL

Keyword(s):

Magnetic Field ◽

Black Holes ◽

Black Hole ◽

Synchrotron Emission ◽

Relativistic Jets ◽

X Ray ◽

Linearly Polarized ◽

Hard State ◽

X Ray Binaries ◽

The Magnetic Field

For most black hole X-ray binaries, the fraction of X-ray flux originating in the synchrotron jets is generally thought to be low in the hard state. However in one intriguing case, the infrared – X-ray correlations, evolution of broadband spectra and timing signatures suggest that synchrotron emission from a jet likely dominated both the infrared and X-ray flux on the hard state decline of an outburst of XTE J1550–564 at a luminosity of ~ (2 × 10-4 – 2 × 10-3) L Edd . Synchrotron emission from the relativistic jets launched close to black holes can be highly linearly polarized, depending on the configuration of the magnetic field. It has recently been shown that the polarimetric signature of their jets is detected in the infrared and is highly variable. This reveals the magnetic geometry in a region of the compact jet near its base, close to the black hole. From these results, it is predicted that in some cases, high (possibly up to 10%), variable levels of X-ray polarization from synchrotron emission originating in jets will be detected from accreting black holes by future spaceborne X-ray polarimeters.

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A public relativistic transfer function model for X-ray reverberation mapping of accreting black holes

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1720 ◽

2019 ◽

Vol 488 (1) ◽

pp. 324-347 ◽

Cited By ~ 14

Author(s):

Adam Ingram ◽

Guglielmo Mastroserio ◽

Thomas Dauser ◽

Pieter Hovenkamp ◽

Michiel van der Klis ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Active Galactic Nuclei ◽

Radial Profile ◽

Galactic Nuclei ◽

Seyfert Galaxy ◽

Geometric Constraints ◽

Time Lags ◽

X Ray ◽

X Ray Binaries

ABSTRACTWe present the publicly available model reltrans that calculates the light-crossing delays and energy shifts experienced by X-ray photons originally emitted close to the black hole when they reflect from the accretion disc and are scattered into our line of sight, accounting for all general relativistic effects. Our model is fast and flexible enough to be simultaneously fit to the observed energy-dependent cross-spectrum for a large range of Fourier frequencies, as well as to the time-averaged spectrum. This not only enables better geometric constraints than only modelling the relativistically broadened reflection features in the time-averaged spectrum, but additionally enables constraints on the mass of supermassive black holes in active galactic nuclei and stellar-mass black holes in X-ray binaries. We include a self-consistently calculated radial profile of the disc ionization parameter and properly account for the effect that the telescope response has on the predicted time lags. We find that a number of previous spectral analyses have measured artificially low source heights due to not accounting for the former effect and that timing analyses have been affected by the latter. In particular, the magnitude of the soft lags in active galactic nuclei may have been underestimated, and the magnitude of lags attributed to thermal reverberation in X-ray binaries may have been overestimated. We fit reltrans to the lag-energy spectrum of the Seyfert galaxy Mrk 335, resulting in a best-fitting black hole mass that is smaller than previous optical reverberation measurements (∼7 million compared with ∼14–26 million M⊙).

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The Formation and Evolution of Black-Hole Binaries

Symposium - International Astronomical Union ◽

10.1017/s0074180900055595 ◽

1996 ◽

Vol 165 ◽

pp. 93-103

Author(s):

Roger W. Romani

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

High Mass ◽

X Ray ◽

Black Hole Binaries ◽

Low Mass ◽

Formation And Evolution ◽

X Ray Binaries ◽

Black Hole Candidates

The presence of accreting black holes (BH) among the X-ray binaries has been recognized for many years. Traditionally, Cyg X-1 and the handful of other candidates have been thought of as cousins of the HMXB neutron star systems. Recent studies of the soft X-ray transients such as A 0620-00 have, however, shown that the dynamical evidence makes these low-mass systems very strong black-hole candidates. Further, analysis of the eventual end-states of various high-mass X-ray binaries suggest that some could end as observable BH-pulsar binaries, although the first such system is yet to be discovered.

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