Relevant bibliographies by topics / Black hole X-ray binaries

Academic literature on the topic 'Black hole X-ray binaries'

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Published: 6 September 2023

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

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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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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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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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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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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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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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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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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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Dissertations / Theses on the topic "Black hole X-ray binaries"

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Klein-Wolt, Marc. "Black hole X-ray binaries." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 2004. http://dare.uva.nl/document/91386.

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EGRON, ELISE MARIE JEANNE. "Spectral Comparisons of Neutron Star Low-Mass X-Ray Binaries with Black Hole X-Ray Binaries." Doctoral thesis, Università degli Studi di Cagliari, 2013. http://hdl.handle.net/11584/266223.

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The study of high-resolution X-ray spectra of neutron star low-mass X-ray binaries (LMXBs) allows the investigation of the innermost parts of the accretion disk and immediate surroundings of the compact object. The weak magnetic eld of old neutron stars present in such systems allows the accretion disk to approach very close to the compact object, like in black hole X-ray binaries. Using data from X-ray satellites such as XMM-Newton, RXTE, and BeppoSAX, I studied the reection component in two neutron star LMXBs: MXB 1728-34 and 4U 1735-44. I showed that the iron line at 6:4
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Dusoye, Avishek. "Accretion and outflow in black-hole x-ray binaries." Master's thesis, University of Cape Town, 2015. http://hdl.handle.net/11427/15518.

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Black hole X-ray binaries (BHXBs) are stellar binary systems consisting of a black hole (BH) and a companion star. They are known to produce X-ray emission through the accretion of mass from the companion star onto the black hole via an accretion disc, as well as radio emission originating from their jets. My thesis splits into two projects. On one hand, I focus on the connection between the X-ray emitting accretion disc and the radio jets of BHXBs in general, by studying the quasi-simultaneous evolution of the radio fluxes and the X-ray fluxes from 17 BHXBs. This connection, also known as the radio/X-ray correlation has been studied and updated over the past years. New observations of new and known sources have shown that another population of X-ray binaries exists (referred to as outliers), lying below the standard radio/X-ray correlation. I investigate whether the mass of the black hole component of BHXBs can explain the existence of these outliers. In my second project, I focus on an exotic source, known as SS433. It has a supercritical accretion disc and displays precessing relativistic jets. I investigate whether these jets are made up of proton-electron plasma or electron-positron plasma. Circular polarization (CP) is a good diagnostics for understanding the particle composition of radio jets. Therefore we have observed the circular polarized flux densities of SS433 using the Australia Telescope Compact Array (ATCA) for a broad range of frequencies between 1:4 - 10 GHz. From those observations, a CP spectrum can be constructed and the spectral index can be estimated. There are 4 ways of producing CP emission and the spectral index helps us to constrain the CP production mechanism. In addition, the kinematics of propelling a proton-electron plasma in a jet is different from that of electronpositron plasma. I simulate various plausible models for the energy content of the jets and thereby aim to constrain the particle composition of the jets. Black hole X-ray binaries (BHXBs) are stellar binary systems consisting of a black hole (BH) and a companion star. They are known to produce X-ray emission through the accretion of mass from the companion star onto the black hole via an accretion disc, as well as radio emission originating from their jets. My thesis splits into two projects. On one hand, I focus on the connection between the X-ray emitting accretion disc and the radio jets of BHXBs in general, by studying the quasi-simultaneous evolution of the radio fluxes and the X-ray fluxes from 17 BHXBs. This connection, also known as the radio/X-ray correlation has been studied and updated over the past years. New observations of new and known sources have shown that another population of X-ray binaries exists (referred to as outliers), lying below the standard radio/X-ray correlation. I investigate whether the mass of the black hole component of BHXBs can explain the existence of these outliers. In my second project, I focus on an exotic source, known as SS433. It has a supercritical accretion disc and displays precessing relativistic jets. I investigate whether these jets are made up of proton-electron plasma or electron-positron plasma. Circular polarization (CP) is a good diagnostics for understanding the particle composition of radio jets. Therefore we have observed the circular polarized flux densities of SS433 using the Australia Telescope Compact Array (ATCA) for a broad range of frequencies between 1:4 - 10 GHz. From those observations, a CP spectrum can be constructed and the spectral index can be estimated. There are 4 ways of producing CP emission and the spectral index helps us to constrain the CP production mechanism. In addition, the kinematics of propelling a proton-electron plasma in a jet is different from that of electron-positron plasma. I simulate various plausible models for the energy content of the jets and thereby aim to constrain the particle composition of the jets.
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Knevitt, Gillian Frances Grace. "Black hole X-ray binaries : radiation and high-redshift feedback." Thesis, University of Leicester, 2014. http://hdl.handle.net/2381/29158.

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The accretion of matter onto black holes results in their characteristic spectrum through which we can identify them and study their properties. Furthermore, this radiation can couple to their surroundings, resulting in complex interactions between black holes and their environments. In this thesis, I study the accreting properties of stellar mass black holes, and examine the effect that such interactions may have had on the early universe. I also consider the observational characteristics of the lowest luminosity stellar mass black hole binary systems in our own galaxy. Approximately one billion years after the Big Bang, the universe underwent a huge baryonic phase change, in which neutral hydrogen became ionized by the first sources of radiation. Massive stars are thought to drive this process, but their ionizing lifetimes could have been extended by a later phase in their evolution: black hole X-ray binary formation. However, the extent of this enhancement is not known, and has been highly debated in recent literature. In this thesis, I show that X-ray binaries were unlikely to be present in sufficient numbers to exert a significant effect on the intergalactic medium. Using a stellar population synthesis model of a single starburst event, I show that radiation from X-ray binaries dominates the ionizing power of a cluster after the most massive stars have ended their lives. However, their high energy spectra and short lifetimes mean their ionizing timescales are too long for them to affect the progress of reionization. Even so, the high escape fraction of X-rays from galaxies still provides scope for low level heating and ionization of the distant intergalactic medium under different circumstances, such as in the context of continuous star formation. I also assess the detectability of the dimmest black hole binary systems in the Milky Way. Using a catalogue of black hole binaries in our galaxy, I find that there is a statistically significant lack of short orbital period systems, when compared to the neutron star binary population. I show that these sources may be hidden from view, rather than being truly absent, due to radiatively inefficient accretion, in which energy is lost to the black hole. However, this conclusion requires that the switch to inefficient accretion occurs sharply at a threshold mass accretion rate. In the case of a smoother switch, alternative observational or evolutionary arguments must be put forward to explain this dearth.
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Shidatsu, Megumi. "Observational Studies of Accretion Disks in Black Hole X-ray Binaries." 京都大学 (Kyoto University), 2015. http://hdl.handle.net/2433/199106.

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Miller, Jon Matthew 1975. "X-ray spectroscopic and timing studies of galactic black hole binaries." Thesis, Massachusetts Institute of Technology, 2002. http://hdl.handle.net/1721.1/29935.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2002.
Includes bibliographical references (p. 183).
In rare cases, optical observations of Galactic binary star systems which are bright in the X-ray portion of the electromagnetic spectrum dynamically constrain the mass of one component to be well above theoretical limits for a neutron star. These systems - and systems with similar X-ray properties - are classified as black hole binaries. In this thesis, I report on observations of black hole binaries made with satellite observatories in the X-ray band. The region closest to the black hole is revealed in X-rays due to the viscous heating of matter that is accreted from the companion star. X-ray observations of these systems may therefore reveal General Relativistic effects. A fundamental and testable prediction of General Relativity is that matter may orbit more closely around black holes with significant angular momentum. I have investigated the possibility of black hole "spin" and the geometry of accretion flows in these systems using X-ray continuum spectroscopy, fast variability studies, and the shape of iron fluorescent emission lines in this band. I present evidence for black hole spin in XTE J1550-564, XTE J1650-500, and XTE J1748-248. Spin is not required by high-resolution spectral analysis of the archetypical Galactic black hole - Cygnus X-1 but a thermal accretion disk plus hot corona geometry is confirmed. Studies of XTE J1118+480 and GRS 1758-258 at low X-ray luminosity reveal that models for radiatively-inefficient accretion do not satisfactorily describe the geometry in these systems.
y Jon Matthew Miller.
Ph.D.
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Brocksopp, Catherine. "Multiwavelength variability of black hole x-ray binaries in the low/hard state." Thesis, [n.p.], 2000. http://oro.open.ac.uk/19112/.

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MARINO, ALESSIO. "Imperfect accretion: ejecting matter in X-ray binaries." Doctoral thesis, Università degli Studi di Palermo, 2021. http://hdl.handle.net/10447/479017.

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X-ray binaries are binary stars composed of a compact object (a black hole, a neutron star) accreting matter from a companion star. These sources can be considered perfect astrophysical laboratories to test our knowledge of, e.g., General Relativity and Magneto-Hydrodynamics. Accretion is the key phenomenon characterizing these systems, but it is not always completely efficient. In many systems, ejections of matter are also observed, e.g. in the form of jets and winds, or also suggested, e.g. to explain the observed strong orbital expansion of a number of systems. Furthermore accretion and ejection seems to be somehow interconnected but the nature of this correlation is not completely clear. The purpose of this thesis is the study of a number of cases where the accretion is imperfect and mass losses have to be taken into account to correctly model the physical properties of the binaries. In the first of the featured projects, I focus on the spectral study of the accretion flow in the Neutron Star (NS) Low Mass X-ray Binary (LMXB) 1RXS J180408.9-342058, an intriguing system which in the past exhibited “very faint” phases of activity. I performed a spectral analysis of data collected by different X-ray telescopes, i.e. INTEGRAL, Swift and NuSTAR, The study led to several interesting results, in particular the observation of the intermediate spectral state, hard to catch in NS LMXBs because very short-lived, and new constraints on the nature of the companion star, which exclude the hypothesis of a helium dwarf companion as suggested in the past. The second project presents a systematic study of (almost) all known Accreting Millisecond X-ray Pulsars (AMXPs), i.e. LMXBs hosting an X-ray pulsar spinning at millisecond periods, with the aim of looking for indications of non-conservative mass-transfer in this class. Comparing this observed luminosity averaged over twenty years with the one expected from the theory in a conservative scenario, I found that over a sample of 19 sources, around one half of it shows indications for mass losses. The third project in this thesis is dedicated to jets, the most known form of mass ejection in X-ray binaries. Jets are characterized by flat radio-to-mid-IR spectra, which have been modelled in the last few decades using the Internal Shocks model ISHEM. The basic idea of this model consists in using the observed X-ray variability as a proxy for the fluctuations of the Lorentz factor in the ejected shells along the jet. I applied the model on the multi-wavelength data set of the NS LMXB 4U 0614+091. I found that ISHEM describes satisfactorily the data only in two cases: using the X-ray variability but in non-conical geometry or either in conical geometry but using flicker noise instead of the X-ray variability. The final project of my thesis aims at testing a unified accretion-ejection model to the Black Hole LMXB MAXI J1820+070. The model considers the accretion flow in X-ray binaries as two-fold, comprising a truncated geometrically thin disk far from the Black Hole and a so-called jet emitting disk serving as the base of the jet close to the Black Hole. Interestingly, the model allows not only to describe the X-rays data, but also to predict the radio power emitted by the jet. In order to test the model, I used X-rays data from Swift and NuSTAR. The preliminary results of the spectral fitting suggest that the model is indeed effective in describing the observed X-ray spectra. Furthermore, the analysis reveals the need for describing the reflection spectrum with two reflection components instead of one: the origin of such intriguing component, if confirmed, will be object of future investigations.
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Dijk, Robertus Cornelis Adrianus van. "Gamma-ray observations of x-ray binaries with COMPTEL a study of black-hole candidates and 2CG 135+01 /." Amsterdam : Utrecht : Amsterdam : Sterrenkundig Instituut "Anton Pannekoek", Universiteit van Amsterdam ; Stichting Ruimteonderzoek Nederland ; Universiteit van Amsterdam [Host], 1996. http://dare.uva.nl/document/91713.

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Burke, Mark J. "Extragalactic X-ray binaries : black holes and neutron stars in Centaurus A." Thesis, University of Birmingham, 2013. http://etheses.bham.ac.uk//id/eprint/4496/.

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This thesis presents research into the X-ray binary population of NGC 5128 (Centaurus A). The two principle investigations focus on the identification of black hole candidates, which can be identified by their long term variability and spectral properties. We demonstrate this with what we believe is our best example; a source that faded over two months of observations and displayed cool disc thermal-dominant spectra when at high luminosities- similar to the Galactic black hole X-ray binaries. The main result of this research is that the population of black hole X-ray binaries is more pronounced in the dust lane of the galaxy compared to in the halo. The explanation of this result, based around the mass of the donor stars required for systems to emit at the observed luminosities, may also explain the long noted effect of a steepening of the X-ray luminosity function in early-type galaxies at a few 10٨38 erg/s; an effect that increases with the age of the stellar population. Finally, frequent Chandra observations of the NGC 5128 were used to investigate the two known ultraluminous X-ray sources. These are transient systems and were observed at luminosities (1-10)% of their peak, in the regime frequented by the Galactic X-ray binaries. This presented an exciting opportunity to study the lower luminosity behaviour of these systems in an effort to determine the mass of the accreting compact object. The results of the spectral analysis point towards accretion powered by a stellar, rather than intermediate mass black hole. The long term variability of these sources is reminiscent of several of the long period Galactic X-ray binaries.
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Books on the topic "Black hole X-ray binaries"

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A, Nowak Michael, and United States. National Aeronautics and Space Administration., eds. X-ray variability coherence: How to compute it, what it means, and how it constrains models of GX 339-4 and Cygnus X-1. [Washington, DC: National Aeronautics and Space Administration, 1997.

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A, Nowak Michael, and United States. National Aeronautics and Space Administration., eds. X-ray variability coherence: How to compute it, what it means, and how it constrains models of GX 339-4 and Cygnus X-1. [Washington, DC: National Aeronautics and Space Administration, 1997.

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A, Nowak Michael, and United States. National Aeronautics and Space Administration., eds. X-ray variability coherence: How to compute it, what it means, and how it constrains models of GX 339-4 and Cygnus X-1. [Washington, DC: National Aeronautics and Space Administration, 1997.

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United States. National Aeronautics and Space Administration., ed. A search for periodicity in the X-ray spectrum of black hole candidate A0620-00. [Washington, DC: National Aeronautics and Space Administration, 1991.

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Investigating the Physics of Hard X-ray Outbursts from the Galactic Center Supermassive Black Hole Sagittarius A*. [New York, N.Y.?]: [publisher not identified], 2016.

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United States. National Aeronautics and Space Administration., ed. Is there a supermassive black hole in the nucleus of M31?: NASA grant NAG5-2673 : final report for the period 15 August 1994 through 14 August 1997. Cambridge, Mass: Smithsonian Institution, Astrophysical Observatory, 1997.

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Shafee, Rebecca. Measuring black hole spin. 2009.

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National Aeronautics and Space Administration (NASA) Staff. Relativistic Astrophysics in Black Hole and Low-Mass Neutron Star X-Ray Binaries. Independently Published, 2018.

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Ho, Luis C., Thomas J. Maccarone, and Robert P. Fender. From X-ray Binaries to Quasars: Black Holes on All Mass Scales. Springer, 2008.

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(Editor), Thomas J. Maccarone, Robert P. Fender (Editor), and Luis C. Ho (Editor), eds. From X-ray Binaries to Quasars: Black Holes on All Mass Scales. Springer, 2006.

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Book chapters on the topic "Black hole X-ray binaries"

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Tanaka, Y. "Black-Hole Binaries." In The Universe in X-Rays, 237–59. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34412-4_16.

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Tauris, T. M., and G. J. Savonije. "Spin-Orbit Couplings in X-Ray Binaries." In The Neutron Star—Black Hole Connection, 337–42. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0548-7_25.

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Gilfanov, M. "X-Ray Emission from Black-Hole Binaries." In The Jet Paradigm, 17–51. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76937-8_2.

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Bildsten, L., and R. E. Rutledge. "Transient Low-Mass X-Ray Binaries in Quiescence." In The Neutron Star—Black Hole Connection, 245–60. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0548-7_14.

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Gilfanov, M., E. Churazov, and R. Sunyaev. "X-ray Spectral Variability of Black Hole Binaries." In Observational Evidence for Black Holes in the Universe, 319–40. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4750-7_23.

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Spruit, H. C. "Gamma-Ray Bursts from Neutron Stars Spun up in X-Ray Binaries." In The Neutron Star—Black Hole Connection, 467–74. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0548-7_33.

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van Paradijs, J. "Black holes in X-ray binaries." In Accretion Disks — New Aspects, 21–35. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/bfb0105818.

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McClintock, Jeffrey E. "Black Holes in Binary Systems." In X-Ray Binaries and Recycled Pulsars, 27–36. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_3.

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Volwerk, Martin, Roeland Oss, and Jan Kuijpers. "Magnetic Flares Near Black Holes." In X-Ray Binaries and Recycled Pulsars, 537. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_47.

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MÉndez, M. "Timing the Kilohertz Quasi-Periodic Oscillations in Low-Mass X-Ray Binaries." In The Neutron Star—Black Hole Connection, 313–18. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0548-7_21.

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Conference papers on the topic "Black hole X-ray binaries"

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Gallo, Elena. "Black hole X-ray binary jets." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130232.

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Nowak, Michael A. "Modeling black hole x-ray power spectra." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45937.

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Mukai, Koji. "Application of magnetic braking theories to black hole binaries." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45992.

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Shahbaz, T., T. Naylor, and P. A. Charles. "The mass of the black hole in A0620-00." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.46029.

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Ebisawa, Ken. "X-ray energy spectra from accretion disks in black hole candidates." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.46000.

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Cesares, J., and P. A. Charles. "The mass of the black hole in GS2023+338/V404 Cygni." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.46026.

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MENOU, KRISTEN. "BLACK HOLE ACCRETION IN TRANSIENT X-RAY BINARIES." In Proceedings of the 2nd KIAS Astrophysics Workshop. WORLD SCIENTIFIC, 2002. http://dx.doi.org/10.1142/9789812777959_0008.

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Belloni, Tomaso M., Sara Motta, Jéro^me Rodriguez, and Phillippe Ferrando. "Black-hole Binaries: Life Begins at 40 keV." In SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE: Proceedings of the 2nd International Simbol-X Symposium. AIP, 2009. http://dx.doi.org/10.1063/1.3149408.

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Grebenev, Sergei A., Rashid A. Sunyaev, and Mikhail N. Pavlinsky. "Observational constraints on the models of disk accretion onto a black hole." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45949.

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Luo, Chuan, Cesar Meirelles, and Edison Liang. "X-ray transitions of black hole binaries and variable α-parameter disks." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45991.

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Reports on the topic "Black hole X-ray binaries"

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Tournear, Derek M. X-ray Bursts in Neutron Star and Black Hole Binaries from USA Data: Detections and Upper Limits. Office of Scientific and Technical Information (OSTI), February 2003. http://dx.doi.org/10.2172/813180.

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Vollrath, Z. Black Hole Accretion and X-Ray Variability in AGN. Office of Scientific and Technical Information (OSTI), September 2004. http://dx.doi.org/10.2172/833107.

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Shabad, Gayane. High-Frequency X-ray Variability Detection in A Black Hole Transient with USA. Office of Scientific and Technical Information (OSTI), October 2000. http://dx.doi.org/10.2172/784707.

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Shabad, G. High-Frequency X-ray Variability Detection in A Black Hole Transient with USA. Office of Scientific and Technical Information (OSTI), June 2018. http://dx.doi.org/10.2172/1454236.

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Reilly, Kaice T. X-Ray Timing and Spectral Observations of Galactic Black Hole Candidate XTE J1550--564 During Outburst. Office of Scientific and Technical Information (OSTI), December 2002. http://dx.doi.org/10.2172/808722.

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