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Journal articles on the topic 'Black hole X-ray binaries'

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Published: 6 September 2023

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1

Tanaka, Y. "Observation of Black Holes in X-ray Binaries." Symposium - International Astronomical Union 195 (2000): 37–47. http://dx.doi.org/10.1017/s007418090016276x.

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Recent results of X-ray observations of Galactic X-ray binaries containing black holes are reviewed. So far, eleven X-ray binaries are confirmed to contain a black hole based on the mass determined from the optical mass functions. Study of these X-ray binaries shows that accreting black holes exhibit a characteristic X-ray spectrum that is distinct from that of accreting neutron stars. In total, about two dozen X-ray binaries show this characteristic spectrum and are believed to contain a black hole. Most of them are low-mass X-ray binaries and are transients. The statistics indicate the presence of several hundred or more black holes in quiescent X-ray binaries in our galaxy. The observed properties of accreting black holes are discussed, and other, related subjects are also presented.

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Ziółkowski, Janusz, and Krzysztof Belczyński. "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 6, S275 (September 2010): 329–30. http://dx.doi.org/10.1017/s1743921310016340.

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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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3

van den Heuvel, Edward P. J. "High-Mass X-ray Binaries: progenitors of double compact objects." Proceedings of the International Astronomical Union 14, S346 (August 2018): 1–13. http://dx.doi.org/10.1017/s1743921319001315.

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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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Orosz, Jerome A. "Inventory of black hole binaries." Symposium - International Astronomical Union 212 (2003): 365–71. http://dx.doi.org/10.1017/s0074180900212448.

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A small group of X-ray binaries currently provides the best evidence for the existence of stellar-mass black holes. These objects are interacting binary systems where the X-rays arise from accretion of material onto a compact object (i.e., an object with a radius of less than a few hundred km). In some favourable cases, optical studies of the companion star lead to dynamical mass estimates for both components. In 17 cases, the mass of the compact object in an X-ray binary has been shown to exceed the maximum mass of a stable neutron star (about 3 M⊙), which leads to the conclusion that these objects are black holes. In this contribution I will review the basic properties of these black hole binaries.

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5

Chen, Wen-Cong, and Xiang-Dong Li. "Evolution of black-hole intermediate-mass X-ray binaries." Proceedings of the International Astronomical Union 2, S238 (August 2006): 339–40. http://dx.doi.org/10.1017/s1743921307005340.

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AbstractWe propose a plausible mechanism for orbital angular momentum loss in black-hole intermediate-mass X-ray binaries, assuming that a small fraction of the transferred mass form a circumbinary disc. The disc can effectively drain orbital angular momentum from the binary, leading to the formation of compact black-hole low-mass X-ray binaries. This scenario also suggests the possible existence of luminous, persistent black hole low-mass X-ray binaries.

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6

Ivanova, Natalia. "Evolution of binaries with compact objects in globular clusters." Proceedings of the International Astronomical Union 10, S312 (August 2014): 203–12. http://dx.doi.org/10.1017/s1743921315007826.

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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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7

Romani, Roger W. "The Formation and Evolution of Black-Hole Binaries." Symposium - International Astronomical Union 165 (1996): 93–103. http://dx.doi.org/10.1017/s0074180900055595.

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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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8

Makishima, Kazuo. "Observational evidence for intermediate-mass black holes: ultra-luminous X-ray sources." Proceedings of the International Astronomical Union 2, S238 (August 2006): 209–18. http://dx.doi.org/10.1017/s1743921307004991.

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AbstractIncorporating early data from the Suzaku satellite launched in July 2005, properties of Ultra-Luminous compact X-ray sources (ULXs) were studied in close comparison with those of Galactic and Magellanic black-hole binaries. Based on an analogy between these two types of X-ray sources, ULXs showing power-law type spectra are considered to host Comptonized accretion disks, while those with multicolor-disk type spectra are interpreted to harbor “slim” disks. The analogy also suggests that ULXs are radiating near their Eddington limits, and hence their central black holes are significantly more massive than the ordinary stellar-mass black holes contained in Galactic and Magellanic black-hole binaries. In this sense, ULXs can be regarded as intermediate-mass black holes.

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9

Dotani, Tadayasu. "X-ray Observations of Black-Hole Binaries." Journal of the Korean Physical Society 54, no. 6(1) (June 15, 2009): 2552–65. http://dx.doi.org/10.3938/jkps.54.2552.

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10

Remillard, Ronald A., and Jeffrey E. McClintock. "X-Ray Properties of Black-Hole Binaries." Annual Review of Astronomy and Astrophysics 44, no. 1 (September 2006): 49–92. http://dx.doi.org/10.1146/annurev.astro.44.051905.092532.

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11

King, A. R., U. Kolb, and L. Burderi. "Black Hole Binaries and X-Ray Transients." Astrophysical Journal 464, no. 2 (June 20, 1996): L127—L130. http://dx.doi.org/10.1086/310105.

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12

Bailyn, Charles D. "Black Hole Binaries in Quiescence." Proceedings of the International Astronomical Union 12, S324 (September 2016): 35–38. http://dx.doi.org/10.1017/s1743921317002083.

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AbstractI discuss some of what is known and unknown about the behavior of black hole binary systems in the quiescent accretion state. Quiescence is important for several reasons: 1) the dominance of the companion star in optical and IR wavelengths allows the binary parameters to be robustly determined — as an example, we argue that the longer proposed distance to the X-ray source GRO J1655-40 is correct; 2) quiescence represents the limiting case of an extremely low accretion rate, in which both accretion and jets can be observed; 3) understanding the evolution and duration of the quiescent state is a key factor in determining the overall demographics of X-ray binaries, which has taken on a new importance in the era of gravitational wave astronomy.

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13

Pakull, M. W., K. Beuermann, L. P. Angebault, and L. Bianchi. "Low-Mass X-Ray Binaries in the LMC." International Astronomical Union Colloquium 93 (1987): 689. http://dx.doi.org/10.1017/s0252921100105548.

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AbstractWe report results on three low-mass X-ray binaries (LMXB) in the LMC, obtained with EXOSAT, IUE and ground-based (ESO) telescopes: LMC X-2 which appears to be “Sco X-l”-like, LHG 83 and LHG 87. The latter are two weaker sources first detected in the course of the HEAO-B LMC survey. They have faint optical counterparts of which LHG 87 was only recently identified by us. In X-rays, they are characterized by ultrasoft X-ray spectra possibly characteristic of black-hole primaries. LHG 83 furthermore shows evidence for X-ray ionization of the surrounding interstellar medium, similar to the He III region around the black-hole candidate LMC X-l. X-ray binaries with masses of compact objects in excess of 3 M⊙ and ultrasoft X-ray spectra are comparatively frequent in the LMC. We suggest that subcritical accretion onto black holes takes place in LHG 83 and LHG 87.

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14

Van Der Klis, M. "Low-Mass X-ray Binaries—Recent Developments." Symposium - International Astronomical Union 165 (1996): 301–12. http://dx.doi.org/10.1017/s0074180900055765.

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Recent developments in the field of low-mass X-ray binaries are briefly reviewed, with particular emphasis on a comparison between the systems that contain accreting low magnetic-field neutron stars and those that contain black-hole candidates. The possibility that inclination effects play a role in black-hole candidate phenomenology is explored.

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15

LEE, CHANG-HWAN, and GERALD E. BROWN. "ON THE THEORY OF GAMMA RAY BURSTS AND HYPERNOVAE: THE BLACK HOLE SOFT X-RAY TRANSIENT SOURCES." International Journal of Modern Physics A 18, no. 04 (February 10, 2003): 527–76. http://dx.doi.org/10.1142/s0217751x03012266.

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We show that a common evolutionary history can produce the black hole binaries in the Galaxy in which the black holes have masses of ~ 5 - 10M⊙. In the black hole binaries with low-mass, ≲ 2.5M⊙ ZAMS (zero age main sequence) companions, the latter remain in main sequence during the active stage of soft X-ray transients (SXT's), most of them being of K or M classification. In two intermediate cases, IL Lupi and Nova Scorpii with ZAMS ~ 2.5M⊙ companions the orbits are greatly widened because of large mass loss in the explosion forming the black hole, and whereas these companions are in late main sequence evolution, they are close to evolving. Binaries with companion ZAMS masses ≳ 3M⊙ are initially "silent" until the companion begins evolving across the Herzsprung gap. We provide evidence that the narrower, shorter period binaries, with companions now in main sequence, are fossil remnants of gamma ray bursters (GRB's). We also show that the GRB is generally accompanied by a hypernova explosion (a very energetic supernova explosion). We further show that the binaries with evolved companions are good models for some of the ultraluminous X-ray sources (ULX's) recently seen by Chandra in other galaxies. The great regularity in our evolutionary history, especially the fact that most of the companions of ZAMS mass ≲ 2.5M⊙ remain in main sequences as K or M stars can be explained by the mass loss in common envelope evolution to be Case C; i.e. to occur only after core He burning has finished. Since our argument for Case C mass transfer is not generally understood in the community, we add an appendix, showing that with certain assumptions which we outline we can reproduce the regularities in the evolution of black hole binaries by Case C mass transfer.

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16

Zwart, Simon Portegies, Frank Verbunt, and Ene Ergma. "Formation of Low-Mass Black Hole X-Ray Transients." Highlights of Astronomy 11, no. 2 (1998): 775–78. http://dx.doi.org/10.1017/s153929960001875x.

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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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17

Poutanen, Juri, Alexandra Veledina, Andrei V. Berdyugin, Svetlana V. Berdyugina, Helen Jermak, Peter G. Jonker, Jari J. E. Kajava, et al. "Black hole spin–orbit misalignment in the x-ray binary MAXI J1820+070." Science 375, no. 6583 (February 25, 2022): 874–76. http://dx.doi.org/10.1126/science.abl4679.

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The observational signatures of black holes in x-ray binary systems depend on their masses, spins, accretion rate, and the misalignment angle between the black hole spin and the orbital angular momentum. We present optical polarimetric observations of the black hole x-ray binary MAXI J1820+070, from which we constrain the position angle of the binary orbital. Combining this with previous determinations of the relativistic jet orientation, which traces the black hole spin, and the inclination of the orbit, we determine a lower limit of 40° on the spin-orbit misalignment angle. The misalignment must originate from either the binary evolution or black hole formation stages. If other x-ray binaries have similarly large misalignments, these would bias measurements of black hole masses and spins from x-ray observations.

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18

Swank, J. H. "Millisecond Time Variations of X-Ray Binaries." Symposium - International Astronomical Union 188 (1998): 107–10. http://dx.doi.org/10.1017/s0074180900114548.

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Millisecond time-scales are natural for some neutron star and black hole processes, although possibly difficult to observe. The Rossi X-Ray Timing Explorer (RXTE) has found that for the neutron stars in low-mass X-ray binaries (LMXB) there are flux oscillations at high frequencies, with large amplitudes. Z sources and bursters tend to exhibit oscillations in the range 300-1200 Hz. Persistent emission may exhibit one or both of two features. In bursts from different bursters, a nearly coherent pulsation is seen, which may be the rotation period of the neutron star. For some the frequency equals the difference between the two higher frequencies, suggesting a beat frequency model, but in others it is twice the difference. The sources span two orders of magnitude in accretion rate, yet the properties are similar. The similar maximum frequencies suggests that it corresponds to the Kepler orbit frequency at the minimum stable orbit or the neutron star surface, either of which would determine the neutron star masses, radii and equation of state. Theories of accretion onto black holes predict a quasi-periodic oscillation (QPO) related to the inner accretion disk. The two microquasar black hole candidates (BHCs) have exhibited candidates for this or related frequencies.

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Shao, Yong, and Xiang-Dong Li. "Population Synthesis of Black Hole X-Ray Binaries." Astrophysical Journal 898, no. 2 (August 3, 2020): 143. http://dx.doi.org/10.3847/1538-4357/aba118.

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20

Kalogera, Vassiliki. "Donor Stars in Black Hole X‐Ray Binaries." Astrophysical Journal 521, no. 2 (August 20, 1999): 723–34. http://dx.doi.org/10.1086/307562.

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21

Malzac, J. "Spectral components in black hole X-ray binaries." Astronomische Nachrichten 337, no. 4-5 (May 2016): 391–97. http://dx.doi.org/10.1002/asna.201612319.

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Tanaka, Y. "Recent Ginga Results on Galactic X-Ray Binaries." Highlights of Astronomy 9 (1992): 211–15. http://dx.doi.org/10.1017/s1539299600008947.

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AbstractBased on the recent Ginga results, following topics on X-ray binaries are briefly discussed: The cyclotron resonnance features observed from several X-ray pulsars, and related problem of the magnetic field decay. Search for millisec. pulsations from LMXRBs. Very bright transients which are suspected to be new black hole candidates, and an estimation of the number of such black hole sources in our galaxy.

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23

Mahto, Dipo, Md Shams Nadeem, Mahendra Ram, and Kumari Vineeta. "Gravitational Force between the Black Hole and Light Particle in XRBs." Journal of Gravity 2013 (July 9, 2013): 1–6. http://dx.doi.org/10.1155/2013/232676.

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The present research paper derives a formula for gravitational force acting between the black hole and light particle passing near the radius of event horizon of black holes and calculates also their values of different test black holes existing in only X-ray binaries (XRBs).

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Langer, N., C. Schürmann, K. Stoll, P. Marchant, D. J. Lennon, L. Mahy, S. E. de Mink, et al. "Properties of OB star−black hole systems derived from detailed binary evolution models." Astronomy & Astrophysics 638 (June 2020): A39. http://dx.doi.org/10.1051/0004-6361/201937375.

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Context. The recent gravitational wave measurements have demonstrated the existence of stellar mass black hole binaries. It is essential for our understanding of massive star evolution to identify the contribution of binary evolution to the formation of double black holes. Aims. A promising way to progress is investigating the progenitors of double black hole systems and comparing predictions with local massive star samples, such as the population in 30 Doradus in the Large Magellanic Cloud (LMC). Methods. With this purpose in mind, we analysed a large grid of detailed binary evolution models at LMC metallicity with initial primary masses between 10 and 40 M⊙, and identified the model systems that potentially evolve into a binary consisting of a black hole and a massive main-sequence star. We then derived the observable properties of such systems, as well as peculiarities of the OB star component. Results. We find that ∼3% of the LMC late-O and early-B stars in binaries are expected to possess a black hole companion when stars with a final helium core mass above 6.6 M⊙ are assumed to form black holes. While the vast majority of them may be X-ray quiet, our models suggest that these black holes may be identified in spectroscopic binaries, either by large amplitude radial velocity variations (≳50 km s−1) and simultaneous nitrogen surface enrichment, or through a moderate radial velocity (≳10 km s−1) and simultaneous rapid rotation of the OB star. The predicted mass ratios are such that main-sequence companions can be excluded in most cases. A comparison to the observed OB+WR binaries in the LMC, Be and X-ray binaries, and known massive black hole binaries supports our conclusion. Conclusions. We expect spectroscopic observations to be able to test key assumptions in our models, with important implications for massive star evolution in general and for the formation of double black hole mergers in particular.

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Mahto, Di Po, Rama Nand Mehta, Umakant Prasad, Krishna Murari Singh, and Mirza Sarfaraz Hussain John. "Internal Energy of the Non-Spinning Black Holes." Advanced Materials Research 787 (September 2013): 681–86. http://dx.doi.org/10.4028/www.scientific.net/amr.787.681.

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The present paper derives an expression for internal energy of the Non-spinning black holes using first law of black hole thermodynamics and calculates their values of different test Non-spinning holes existing in X-ray binaries (XRBs) and Active Galactic Nuclei (AGN).

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Heinz, Sebastian, and Andrea Merloni. "Exploring Regimes in Black Hole Scaling." Proceedings of the International Astronomical Union 8, S290 (August 2012): 29–36. http://dx.doi.org/10.1017/s174392131201914x.

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AbstractRecent observational evidence suggests the existence of two tracks in the radio-X-ray relation for X-ray binaries. Claims have also been made for deviations from the so-called fundamental plane of black hole activity due to the influence of radiative cooling on synchrotron emission from jets and the relative importance of disk and jet emission. In addition, cases of strongly boosted classes of objects, such as BL Lacs, show evidence for jet emission in their location relative to the fundamental plane. In light of the recent literature activity discussing these issues, we revisit the scaling relations expected for synchrotron emission from jet cores. We review the set of scaling laws expected for different types of emission and discuss their relevance to the new observational data, and the conditions under which breaks in the observed scaling relations should be expected. None of the canonical cases offer a satisfactory explanation for the best fit slope of the steep branch of the radio-X-ray relation in hard-state X-ray binaries.

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PAREDES, J. M. "VHE GAMMA-RAYS FROM GALACTIC X-RAY BINARY SYSTEMS." International Journal of Modern Physics D 17, no. 10 (September 2008): 1849–58. http://dx.doi.org/10.1142/s0218271808013480.

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The detection of TeV gamma-rays from LS 5039 and the binary pulsar PSR B1259–63 by HESS, and from LS I +61 303 and the stellar-mass black hole Cygnus X-1 by MAGIC, provides clear evidence of very efficient acceleration of particles to multi-TeV energies in X-ray binaries. These observations demonstrate the richness of nonthermal phenomena in compact galactic objects containing relativistic outflows or winds produced near black holes and neutron stars. I review here some of the main observational results on very high energy (VHE) γ-ray emission from X-ray binaries, as well as some of the proposed scenarios to explain the production of VHE γ-rays. I put special emphasis on the flare TeV emission, suggesting that the flaring activity might be a common phenomena in X-ray binaries.

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Mirabel, I. F. "Black holes formed by direct collapse: observational evidences." Proceedings of the International Astronomical Union 12, S324 (September 2016): 303–6. http://dx.doi.org/10.1017/s1743921316012904.

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AbstractBinary black holes as the recently detected sources of gravitational waves can be formed from massive stellar binaries in the field or by dynamical interactions in clusters of high stellar density, if the black holes are the remnants of massive stars that collapsed without natal kicks that would disrupt the binary system or eject the black holes from the cluster before binary black hole formation. Here are summarized and discussed the kinematics in three dimensions of space of five Galactic black hole X-ray binaries. For Cygnus X-1 and GRS 1915+105 it is found that the black holes of ~15 M⊙ and ~10 M⊙ in these sources were formed in situ, without energetic kicks. These observations suggest that binary black holes with components of ~10 M⊙ may have been prolifically produced in the universe.

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Salvesen, Greg, and Jonah M. Miller. "Black hole spin in X-ray binaries: giving uncertainties an f." Monthly Notices of the Royal Astronomical Society 500, no. 3 (October 27, 2020): 3640–66. http://dx.doi.org/10.1093/mnras/staa3325.

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ABSTRACT The two established techniques for measuring black hole spin in X-ray binaries often yield conflicting results, which must be resolved before either method may be deemed robust. In practice, black hole spin measurements based on fitting the accretion disc continuum effectively do not marginalize over the colour-correction factor fcol. This factor parametrizes spectral hardening of the disc continuum by the disc atmosphere, whose true properties are poorly constrained. We incorporate reasonable systematic uncertainties in fcol into the eight (non-maximal) black hole spin measurements vetted by the disc continuum fitting community. In most cases, an fcol uncertainty of ±0.2–0.3 dominates the black hole spin error budget. We go on to demonstrate that plausible departures in fcol values from those adopted by the disc continuum fitting practitioners can bring the discrepant black hole spins into agreement with those from iron line modelling. Systematic uncertainties in fcol, such as the effects of strong magnetization, should be better understood before dismissing their potentially dominant impact on the black hole spin error budget.

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Bleach, James. "Pre-low-mass X-ray binaries containing a black hole: investigating a detection mechanism." Open Physics 5, no. 1 (January 1, 2007): 1–10. http://dx.doi.org/10.2478/s11534-006-0035-9.

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AbstractThis work investigates the feasibility of detecting close, detached, black hole-red dwarf binaries, which are expected to be evolutionary precursors of low-mass X-ray binaries (LMXBs). Although this pre-low-mass X-ray binary (pre-LMXB) phase of evolution is predicted theoretically, as yet no such systems have been identified observationally. The calculations presented here suggest that the X-ray luminosity of black hole wind accretion in a pre-LMXB system could exceed the intrinsic X-ray luminosity of the red dwarf secondary star, thereby providing a detection mechanism. However, there is significant uncertainty regarding the efficiency of the conversion of gravitational potential energy to X-ray luminosity resulting from accretion onto a black hole, for example energy may be lost via advection across the event horizon. Still, sources with X-ray luminosities greater than that expected for a red dwarf star, but whose positions coincide with that of a red dwarf would represent candidate pre-LMXB systems. These candidates should be surveyed for the radial velocity shifts that would occur as a result of the orbital motion of a red dwarf star within a close binary system containing a black hole.

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Graham, Alister W., Roberto Soria, Benjamin L. Davis, Mari Kolehmainen, Thomas Maccarone, James Miller-Jones, Christian Motch, and Douglas A. Swartz. "Central X-Ray Point Sources Found to Be Abundant in Low-mass, Late-type Galaxies Predicted to Contain an Intermediate-mass Black Hole." Astrophysical Journal 923, no. 2 (December 1, 2021): 246. http://dx.doi.org/10.3847/1538-4357/ac34f4.

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Abstract Building upon three late-type galaxies in the Virgo cluster with both a predicted black hole mass of less than ∼105 M ⊙ and a centrally located X-ray point source, we reveal 11 more such galaxies, more than tripling the number of active intermediate-mass black hole candidates among this population. Moreover, this amounts to a ∼36 ± 8% X-ray detection rate (despite the sometimes high, X-ray-absorbing, H i column densities), compared to just 10 ± 5% for (the largely H i-free) dwarf early-type galaxies in the Virgo cluster. The expected contribution of X-ray binaries from the galaxies’ inner field stars is negligible. Moreover, given that both the spiral and dwarf galaxies contain nuclear star clusters, the above inequality appears to disfavor X-ray binaries in nuclear star clusters. The higher occupation, or rather detection, fraction among the spiral galaxies may instead reflect an enhanced cool gas/fuel supply and Eddington ratio. Indeed, four of the 11 new X-ray detections are associated with known LINERs or LINER/H ii composites. For all (four) of the new detections for which the X-ray flux was strong enough to establish the spectral energy distribution in the Chandra band, it is consistent with power-law spectra. Furthermore, the X-ray emission from the source with the highest flux (NGC 4197: L X ≈ 1040 erg s−1) suggests a non-stellar-mass black hole if the X-ray spectrum corresponds to the “low/hard state”. Follow-up observations to further probe the black hole masses, and prospects for spatially resolving the gravitational spheres of influence around intermediate-mass black holes, are reviewed in some detail.

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Motta, S. E., J. Rodriguez, E. Jourdain, M. Del Santo, G. Belanger, F. Cangemi, V. Grinberg, et al. "The INTEGRAL view on black hole X-ray binaries." New Astronomy Reviews 93 (December 2021): 101618. http://dx.doi.org/10.1016/j.newar.2021.101618.

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Li, Xiang-Dong. "Evolution of Intermediate-Mass Black Hole X-Ray Binaries." Astrophysical Journal 616, no. 2 (October 22, 2004): L119—L122. http://dx.doi.org/10.1086/426669.

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34

Russell, D. M., S. Markoff, P. Casella, A. G. Cantrell, R. Chatterjee, R. P. Fender, E. Gallo, et al. "Jet spectral breaks in black hole X-ray binaries." Monthly Notices of the Royal Astronomical Society 429, no. 1 (December 10, 2012): 815–32. http://dx.doi.org/10.1093/mnras/sts377.

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35

Zhang, S. N., Wei Cui, and Wan Chen. "Black Hole Spin in X-Ray Binaries: Observational Consequences." Astrophysical Journal 482, no. 2 (June 20, 1997): L155—L158. http://dx.doi.org/10.1086/310705.

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36

Li, Xiang-Dong. "Formation of black hole low-mass X-ray binaries." New Astronomy Reviews 64-66 (February 2015): 1–6. http://dx.doi.org/10.1016/j.newar.2015.02.001.

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37

Truss, M. R. "Super-Eddington Accretion in Black Hole X-Ray Binaries." International Astronomical Union Colloquium 194 (July 2004): 60–62. http://dx.doi.org/10.1017/s0252921100151917.

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AbstractI present, very high resolution hydrodynamical simulations of accretion discs in black hole X-ray binaries accreting near the Eddington limit, including the effects of disc irradiation and mass loss. I show that the extreme variability displayed by sources such as GRS 1915+105 can be explained within the framework of an outburst in a partially irradiated, turbulent, disc.

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38

Brown, G. E., A. Heger, N. Langer, C. H. Lee, S. Wellstein, and H. A. Bethe. "Formation of high mass X-ray black hole binaries." New Astronomy 6, no. 7 (October 2001): 457–70. http://dx.doi.org/10.1016/s1384-1076(01)00077-x.

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39

Cannizzo, J. K. "Disk Instabilities in the Black Hole Binaries." International Astronomical Union Colloquium 158 (1996): 135–38. http://dx.doi.org/10.1017/s025292110003846x.

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I will briefly review recent progress in our understanding of the global propagation of accretion disk instabilities operating in interacting binary systems in which the accreting star is a ~ 10 M⊙ black hole. A detailed discussion of this work can be found in Cannizzo, Chen & Livio (1995).The X-ray light curves of the brightest and best studied X-ray novae – systems such as A0620–00, GS2000+25, GS1124–68, and GRO J0422+32 – are notable in two respects: the rise times are fast (a few days) and the decays have an exponential character, where the e–folding time constant is about 30 to 40 d (Mineshige, Yamasaki, & Ishizaka 1993, hereafter MYI). It is noteworthy that outbursts in dwarf novae also decay exponentially, with the time constant being about a factor of 10 shorter. In this contribution I will discuss the constraints on the physics of accretion disks which the (observed) exponential decay enables us to make.

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Barnard, R. "Big Game Hunting in the Andromeda Galaxy: Identifying and Weighing Black Holes in Low Mass X-Ray Binaries." International Astronomical Union Colloquium 194 (2004): 71–72. http://dx.doi.org/10.1017/s0252921100151954.

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AbstractWe have devised a new technique for identifying stellar mass black holes in low mass X-ray binaries, and have applied it to XMM-Newton observations of two X-ray sources in M31. In particular we search for low accretion rate power density spectra; these are very similar for all LMXB, whether the primary is a black hole or a neutron star. Galactic neutron star LMXB exhibit these distinctive PDS at very low luminosities (~ 1036 erg s–1) while black hole LMXB can exhibit them at luminosities > 1038 erg s–1! Following the work of van der Klis (1994), we assume a maximum accretion rate (as a fraction of the Eddington limit) for low accretion rate PDS that is constant for all LMXB, and obtain an empirical value of ~10% Eddington. We have so far discovered two candidate black hole binaries in M31, exhibiting low accretion rate PDS at up to 3 x 1038 and 5 x 1037 erg s–1. If we assume that they are at <10% Eddington, they have minimum masses of 20 and 4 M⊙ respectively. Furthermore, any LMXB exhibiting a low accretion rate power density spectrum at a luminosity > 5 x 1037 erg s–1 is likely to have a black hole primary.

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van Oers, Pieter, and Sera Markoff. "GRS1915+105: a comparison of the plateau state to the canonical hard state." Proceedings of the International Astronomical Union 6, S275 (September 2010): 294–98. http://dx.doi.org/10.1017/s1743921310016194.

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AbstractGRS 1915+105 is a very peculiar black hole binary that exhibits accretion-related states that are not observed in any other stellar-mass black hole system. One of these states, however – referred to as the plateau state – may be related to the canonical hard state of black hole X-ray binaries. Both the plateau and hard state are associated with steady, relatively lower X-ray emission and flat/inverted radio emission, that is sometimes resolved into compact, self-absorbed jets. To investigate the relationship between the plateau and the hard state, we fit two multi-wavelength observations using a steady-state outflow-dominated model, developed for hard state black hole binaries. The data sets consist of quasi-simultaneous observations in radio, near-infrared and X-ray bands. Interestingly, we find both significant differences between the two plateau states, as well as between the best-fit model parameters and those representative of the hard state. We discuss our interpretation of these results, and the possible implications for GRS 1915+105's relationship to canonical black hole candidates.

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42

Zhang, Youxi. "Stellar-mass black hole spinning and its relation to transient jets." Theoretical and Natural Science 5, no. 1 (May 25, 2023): 418–22. http://dx.doi.org/10.54254/2753-8818/5/20230261.

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Despite the vast research on spinning black holes and jets, little is known about details of jet formation. This paper is aimed to study whether Penroses prediction that black hole spin power jets can be verified. Once proved, a deeper understanding of energy/momentum transfer near event horizon is to be achieved. This paper compares two dominant spin measuring methods. Thermal continuum fitting method makes use of thermal emission to measure the spin, where a theoretical flux profile is created by inputting parameters (inclination of X-ray binaries, distance of X-ray binaries from the earth, mass of black hole, etc). X-ray reflection method uses broadened Fe-line to measure the spin, and that corona geometry is often required. This paper also compares various definitions of jet power and spin-jets relation. In conclusion, transient jets are highly possible to be powered by black hole spin, but more evidence is required to confirm this. Steady jets remain in a vague relation with spin. It has also been found that different measuring methods of both spin and jets can affect the spin-jets relation.

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43

Casares, Jorge. "Observational evidence for stellar-mass black holes." Proceedings of the International Astronomical Union 2, S238 (August 2006): 3–12. http://dx.doi.org/10.1017/s1743921307004590.

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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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Belloni, Tomaso M. "QPO-jet relation in X-ray binaries." Proceedings of the International Astronomical Union 5, H15 (November 2009): 243–44. http://dx.doi.org/10.1017/s174392131000904x.

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AbstractIn the past years, a clear picture of the evolution of outbursts of black-hole X-ray binaries has emerged. While the X-ray properties can be classified into our distinct states, based on spectral and timing properties, the observations in the radio band have shown strong links between accretion and ejection properties. Here I briefly outline the association between X-ray timing and jet properties.

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MIGLIARI, SIMONE, GABRIELE GHISELLINI, JAMES MILLER-JONES, and DAVID RUSSELL. "JET MODELS FOR NEUTRON STAR X-RAY BINARIES." International Journal of Modern Physics: Conference Series 08 (January 2012): 108–13. http://dx.doi.org/10.1142/s2010194512004485.

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A variety of different models for jet formation have been developed over the years (mainly) for black hole systems and young stellar objects. Conclusive observational constraints which would favor one particular mechanism are difficult to obtain. Neutron star X-ray binaries are crucial for advancing our understanding of jet formation in general, building a bridge between the two most studied jet-producing classes of systems: black holes, i.e. non-magnetized, relativistic objects, and young stellar objects, i.e. non-relativistic, magnetized stars. I will briefly review the status of our observational knowledge of jets in neutron star X-ray binaries, with a focus on the parameters which might be involved in the production of jets. I will present recent works and current observational programs aiming to quantify the role of the compact object in the formation of jets in neutron star systems. Finally, I will test a jet model developed for young stellar objects, the X–wind model, on a neutron star system.

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46

Xie, Fu-Guo. "Radiative efficiency of hot accretion flow and the radio/X-ray correlation in X-ray binaries." Proceedings of the International Astronomical Union 10, S312 (August 2014): 139–40. http://dx.doi.org/10.1017/s1743921315007723.

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AbstractSignificant progresses have been made since the discovery of hot accretion flow, a theory successfully applied to the low-luminosity active galactic nuclei (LLAGNs) and black hole (BH) X-ray binaries (BHBs) in their hard states. Motivated by these updates, we re-investigate the radiative efficiency of hot accretion flow. We find that, the brightest regime of hot accretion flow shows a distinctive property, i.e. it has a constant efficiency independent of accretion rates, similar to the standard thin disk. For less bright regime, the efficiency has a steep positive correlation with the accretion rate, while for faint regime typical of advection-dominated accretion flow, the correlation is shadower. This result can naturally explain the observed two distinctive correlations between radio and X-ray luminosities in black hole X-ray binaries. The key difference in systems with distinctive correlations could be the viscous parameter, which determines the critical luminosity of different accretion modes.

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47

Soleri, Paolo, and Rob Fender. "On the nature of the “radio quiet” black hole binaries." Proceedings of the International Astronomical Union 6, S275 (September 2010): 265–69. http://dx.doi.org/10.1017/s1743921310016133.

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AbstractThe accretion/ejection coupling in accreting black hole binaries has been described by empirical relations between the X-ray/radio and X-ray/optical-infrared luminosities. These correlations were initially supposed to be universal. However, recently many sources have been found to produce jets that, given certain accretion-powered luminosities, are fainter than expected from the correlations. This shows that black holes with similar accretion flows can produce a broad range of outflows in power Here we discuss whether typical parameters of the binary system, as well as the properties of the outburst, produce any effect on the energy output in the jet. We also define a jet-toy model in which the bulk Lorentz factor becomes larger than ~1 above ~0.1% of the Eddington luminosity. We finally compare the “radio quiet” black holes with the neutron stars.

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48

Caballero-Garcia, M. D., S. E. Motta, T. M. Belloni, and A. Wolter. "The aperiodic variability of the Ultraluminous X-ray source in NGC 5408." Proceedings of the International Astronomical Union 8, S290 (August 2012): 13–16. http://dx.doi.org/10.1017/s1743921312019102.

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AbstractUltra-Luminous X-ray sources are accreting black holes that might represent strong evidence of the Intermediate Mass Black Holes (IMBH), proposed to exist by theoretical studies but with no firm detection (as a class) so far. We analyze the best X-ray timing and spectral data from the ULX in NGC 5408 provided by XMM-Newton. The main goal is to study the broad-band noise variability of the source. We found an anti-correlation of the fractional root-mean square variability versus the intensity of the source, similar to black-hole binaries during hard states.

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Qin, Y., T. Fragos, G. Meynet, P. Marchant, V. Kalogera, J. Andrews, M. Sørensen, and H. F. Song. "The black hole spin in coalescing binary black holes and high-mass X-ray binaries." Proceedings of the International Astronomical Union 14, S346 (August 2018): 426–32. http://dx.doi.org/10.1017/s1743921318007469.

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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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Zhang, Shuang Nan. "Similar phenomena at different scales: black holes, the Sun, γ-ray bursts, supernovae, galaxies and galaxy clusters." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 41–62. http://dx.doi.org/10.1017/s1743921307009842.

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AbstractMany similar phenomena occur in astrophysical systems with spatial and mass scales different by many orders of magnitudes. For examples, collimated outflows are produced from the Sun, proto-stellar systems, gamma-ray bursts, neutron star and black hole X-ray binaries, and supermassive black holes; various kinds of flares occur from the Sun, stellar coronae, X-ray binaries and active galactic nuclei; shocks and particle acceleration exist in supernova remnants, gamma-ray bursts, clusters of galaxies, etc. In this report I summarize briefly these phenomena and possible physical mechanisms responsible for them. I emphasize the importance of using the Sun as an astrophysical laboratory in studying these physical processes, especially the roles magnetic fields play in them; it is quite likely that magnetic activities dominate the fundamental physical processes in all of these systems.As a case study, I show that X-ray lightcurves from solar flares, black hole binaries and gamma-ray bursts exhibit a common scaling law of non-linear dynamical properties, over a dynamical range of several orders of magnitudes in intensities, implying that many basic X-ray emission nodes or elements are inter-connected over multi-scales. A future high timing and imaging resolution solar X-ray instrument, aimed at isolating and resolving the fundamental elements of solar X-ray lightcurves, may shed new lights onto the fundamental physical mechanisms, which are common in astrophysical systems with vastly different mass and spatial scales. Using the Sun as an astrophysical laboratory, “Applied Solar Astrophysics” will deepen our understanding of many important astrophysical problems.

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