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Готові списки джерел за темами / Galactic binaries

Добірка наукової літератури з теми "Galactic binaries"

Автор: Grafiati

Опубліковано: 22 жовтня 2022

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Статті в журналах з теми "Galactic binaries":

1

Christiansen, Hugo R. "Neutrino signals from galactic binaries." Brazilian Journal of Physics 37, no. 2b (July 2007): 642–47. http://dx.doi.org/10.1590/s0103-97332007000400031.

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2

Belczynski, Krzysztof, and Ronald E. Taam. "Galactic Populations of Ultracompact Binaries." Astrophysical Journal 603, no. 2 (March 10, 2004): 690–96. http://dx.doi.org/10.1086/381491.

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3

Cornish, Neil J., and Edward K. Porter. "Detecting galactic binaries with LISA." Classical and Quantum Gravity 22, no. 18 (August 24, 2005): S927—S933. http://dx.doi.org/10.1088/0264-9381/22/18/s06.

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4

Bonanos, Alceste Z. "Massive extragalactic eclipsing binaries." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 198. http://dx.doi.org/10.1017/s1743921307010113.

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Masses, radii and luminosities of distant stars can only be measured accurately in eclipsing binaries. The most massive eclipsing binary currently known is WR 20a, which consists of two ~ 80 M⊙ stars in a 3.7 d orbit. Analogs of WR 20a are bound to exist both in massive stellar clusters in our Galaxy and in nearby galaxies. The nearest ones are located in the clusters near the Galactic Center: the Center, Arches, and Quintuplet clusters. The severe amount of reddening in the galactic disk makes the study of galactic clusters challenging. However, with current 8-m class telescopes, the study of massive stars in nearby galaxies is also feasible. The nearest Local Group galaxies (LMC, SMC, M 31, M 33) provide the perfect laboratory for studying massive stars and determining their properties as a function of metallicity. Such studies will constrain models, confirm the dependence of evolution on metallicity and help understand the rate and nature of supernovae and gamma-ray bursts.

5

Witt, H. J., and S. Mao. "Microlensing With Binaries And Planets." Symposium - International Astronomical Union 173 (1996): 233–34. http://dx.doi.org/10.1017/s0074180900231379.

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The ongoing microlensing experiments have now discovered more than 70 candidate events (Alcock et al. 1993, Bennett et al. 1994, Aubourg et al. 1993, Udalski et al. 1994). These experiments have put important constraints on the dark matter content of the Galactic halo (Alcock et al. 1995a) and yielded many interesting results about Galactic structure (Paczyński et al. 1994, Stanek et al. 1994).

6

van der Hucht, Karel A., and Bambang Hidayat. "Wolf-Rayet Binaries." Symposium - International Astronomical Union 200 (2001): 79–83. http://dx.doi.org/10.1017/s0074180900225084.

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A WR binary frequency of 37% is found in the VIIth Catalogue of Galactic Wolf-Rayet Stars. Indications are that perhaps all WR stars are binaries and thus that all WR stars point to massive binary formation regions.

7

Di Stefano, Rosanne. "Microlensing: A Tool to Probe Distant Binary Populations." Symposium - International Astronomical Union 200 (2001): 529–38. http://dx.doi.org/10.1017/s0074180900225643.

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Programs designed to observe gravitational microlensing are poised to provide a great deal of information about binary populations far from Earth, including those in the Galactic Bulge, in the Magellanic Clouds, in M31, and perhaps in other external galaxies. Because many millions of stars are monitored, microlensing observations allow us to study binaries in three ways: (1) when they are “involved” in a microlensing event (as either a lens or lensed source), (2) when variability due to binarity produces significant variations in the light curve, and (3) when light from a more distant star is attenuated or refracted by matter associated with the binary system (e.g., in a disk).Microlensing observations will discover large numbers of binaries and planetary systems in a variety of galactic environments. Thus, comparative statistical studies of binary properties (distributions of mass ratios and orbital separations) are possible.An intriguing sign that we have already begun to learn about binaries through microlensing observations comes from work indicating that all of the lenses detected to date may in fact be binaries. For observations along the direction of the Magellanic Clouds this would imply that, if the lenses are primarily located in the Halo, then MACHOs tend to be binaries. If, on the other hand, most of the lenses are located in the Magellanic Clouds, microlensing observations are giving us a unique way to explore a distant stellar population of binaries.

8

Stroeer, Alexander, Matthew Benacquista, and Frank Ceballos. "Detecting Double Degenerate Progenitors of SNe Ia with LISA." Proceedings of the International Astronomical Union 7, S281 (July 2011): 217–20. http://dx.doi.org/10.1017/s1743921312015062.

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AbstractThe Galactic population of close white dwarf binaries is expected to provide the largest number of gravitational wave sources for low frequency detectors such as the Laser Interferometer Space Antenna (LISA). Current data analysis techniques have demonstrated the capability of resolving on the order of 104 white dwarf binaries from a 2 year observation. Resolved binaries are either at high frequencies or large amplitudes. Such systems are more likely to be high-mass binaries, a subset of which will be progenitors of SNe Ia in the double degenerate scenario. We report on results of a study of the properties of resolved binaries using a population synthesis model of the Galactic white dwarf binaries and a LISA data analysis algorithm using Mock LISA Data Challenge tools.

9

Zwitter, Tomaž. "GAIA Survey of Galactic Eclipsing Binaries." International Astronomical Union Colloquium 187 (2002): 31–36. http://dx.doi.org/10.1017/s0252921100001196.

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AbstractThe general importance and capabilities of observations of eclipsing binaries by the forthcoming ESA mission GAIA are discussed. Availability of spectroscopic observations and a large number of photometric bands on board will make it possible to reliably determine physical parameters for ∼ 105 binary stars. It is stressed that current methods of object by object analysis will have to be modified and included in an automatic analysis pipeline.

10

Hoang, Bao-Minh, Smadar Naoz, and Melodie Sloneker. "Binary Natal Kicks in the Galactic Center: X-Ray Binaries, Hypervelocity Stars, and Gravitational Waves." Astrophysical Journal 934, no. 1 (July 1, 2022): 54. http://dx.doi.org/10.3847/1538-4357/ac7787.

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Abstract Theoretical and observational studies suggest that stellar binaries exist in large numbers in galactic nuclei like our own Galactic Center. Neutron stars (NSs), and debatedly, black holes and white dwarfs, receive natal kicks at birth. In this work, we study the effect of two successive natal kicks on a population of stellar binaries orbiting the massive black hole (MBH) in our Galactic Center. These natal kicks can significantly alter the binary orbit in a variety of ways, and also the orbit of the binary around the MBH. We found a variety of dynamical outcomes resulting from these kicks, including a steeper cusp of single NSs relative to the initial binary distribution. Furthermore, hypervelocity star and binary candidates, including hypervelocity X-ray binaries, are a common outcome of natal kicks. In addition, we show that the population of X-ray binaries in the Galactic Center can be used as a diagnostic for the BH natal kick distribution. Finally, we estimate the rate of gravitational wave events triggered by natal kicks, including binary mergers and EMRIs.

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Дисертації з теми "Galactic binaries":

1

Pfahl, Eric D. (Eric David) 1976. "The galactic population of binaries containing neutron stars." Thesis, Massachusetts Institute of Technology, 2002. http://hdl.handle.net/1721.1/8487.

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Thesis (Ph.D.)--Massachusetts Institute of Technology, Dept. of Physics, 2002.
Includes bibliographical references (p. 127-140).
The research presented herein is a theoretical investigation of the formation, evolution, and ultimate fate of low-, intermediate-, and high-mass X-ray binaries (L/I/HMXBs). The primary theoretical tool used throughout is binary population synthesis. Results of these calculations are used to account for the numbers and properties of observed X-ray binaries and their descendants, as well as to direct future observational and theoretical work. Combining binary population synthesis and binary stellar evolution calculations, I present a systematic population study of L/IMXBs in the Galactic plane. Since full stellar evolution calculations are used to model the X-ray binary phase, it is possible to make detailed comparisons between the theoretical models and observations. It is demonstrated quantitatively that IMXBs probably play a crucial role in shaping the population of LMXBs observed at the current epoch, as well as their descendant binary millisecond radio pulsars. Recently, a new class of HMXBs has emerged, distinguished from other HMXBs by their wide, nearly circular orbits. I show that the discovery of a significant number of such systems is at odds with the conventional wisdom that most neutron stars receive very large "kick" speeds at birth. This problem may be rectified in a self-consistent way if the kick speed depends on the rotation rate of the pre-collapse core, which I propose is strongly influenced by the evolution of the neutron-star progenitor in a binary system. The reasonable suggestion that certain globular clusters contain nearly 1000 neutron stars conflicts with the large mean kick speeds estimated from observations of isolated radio pulsars, which are 5 to 10 times the present cluster escape speeds.
(cont.) Therefore, most neutron stars born from single progenitors should have been ejected from their host clusters. I show that many more neutron stars are retained if a significant fraction are formed with massive stellar companions, but that the retained fraction is still too small to account for the inferred large numbers of neutron stars at the current epoch. Several alternative hypotheses are discussed, including the intriguing possibility that globular clusters we see today were ten times more massive in the distant past. The Chandra X-ray Observatory has revealed hundreds of previously undetected point sources in a small field about the Galactic center. I show that the majority of these sources may be neutron stars accreting from the winds of unevolved companion stars. Infrared observations are proposed to search for the stellar counterparts of the X-ray sources.
by Eric D. Pfahl.
Ph.D.

2

Homer, Lee. "High-speed photometry of compact x-ray binaries." Thesis, University of Oxford, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.301573.

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3

Cackett, Edward M. "Compact objects in active galactic nuclei and X-ray binaries." Thesis, University of St Andrews, 2007. http://hdl.handle.net/10023/150.

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In this thesis I study the inner-most regions of Active Galactic Nuclei (AGN) using the reverberation mapping technique, and neutron star low-mass X-ray binaries in quiescence using X-ray observations. Using the 13-year optical monitoring data for the AGN NGC 5548, the luminosity dependence of the Hβ emitting radius was modelled using a delay map, finding that the radius scales with luminosity as predicted by recent theoretical models. Time-delays between the continuum at different wavelengths in AGN can be used to probe the accretion disc. Here, continuum time-delays in a sample of 14 AGN were used to measure the radial temperature profile of the accretion discs, determine the nuclear extinction, and measure distances to the objects. However, the distances measured correspond to a value for Hubble's constant that is a factor of ~2 lower than the accepted value. The implications of this on the thermal disc reprocessing model are discussed. I present two Chandra observations of the neutron star transient in the globular cluster NGC 6440 in quiescence, where the power-law component to the spectrum is seen to be variable between the observations, suggesting that there is ongoing residual accretion. From a Chandra observation of the globular cluster Terzan 1, I have identifed the likely quiescent counterpart to a transient previously observed in outburst, and discuss the other sources within the cluster. Using Chandra and XMM-Newton monitoring observations of two neutron star transients (KS 1731-260 and MXB 1659-29) in quiescence I have found that the neutron star crusts in both sources have now returned to thermal equilibrium with the core. These observations also indicate that the crusts in both sources may have a high thermal conductivity and that enhanced neutrino emission may be occurring in the core. Finally, the discovery of an X-ray transient with XMM-Newton is presented, and the other sources in this observation discussed.

4

Shahbaz, Tariq. "Observational studies of Galactic neutron star and black-hole binaries." Thesis, Keele University, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.261527.

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5

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.

6

Iwasa, Mao. "Lidov-Kozai mechanism in shrinking Massive Black Hole binaries." Kyoto University, 2018. http://hdl.handle.net/2433/232233.

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7

Benlloch, García Sara. "Long-term x-ray variability of active galactic nuclei and x-ray binaries." [S.l. : s.n.], 2004. http://www.bsz-bw.de/cgi-bin/xvms.cgi?SWB11051893.

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8

Chaname, Julio. "Topics of galactic structure and stellar and chemical evolution." The Ohio State University, 2005. http://rave.ohiolink.edu/etdc/view?acc_num=osu1126128106.

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9

Rees, Bryan. "A study of planetary nebulae in and towards the Galactic Bulge." Thesis, University of Manchester, 2011. https://www.research.manchester.ac.uk/portal/en/theses/a-study-of-planetary-nebulae-in-and-towards-the-galactic-bulge(ff6c0373-e5a5-491f-b5fb-bda36acac8ba).html.

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A planetary nebula (PN) consists of material, mainly gas, that has been ejected from a star on the asymptotic giant branch of its life cycle. This material emits electromagnetic radiation due to photoionization and recombination, collisional and radiative excitation or free-free radiation. The envelope of material moves outwards from the central star and may take one of a variety of shapes. These shapes are believed to be sculpted by the stellar wind, magnetic fields and interactions with a binary companion. However, within a time scale of as little as 10 000 years the nebula fades from view and merges with the interstellar medium.Similar variations in the shape of planetary nebulae (PNe) can be seen in both the Galactic Bulge and Disc and in the Magellanic Clouds. It is therefore reasonable to assume that the shaping process is universal. By classifying PNe by morphology and relating those shapes to other nebular properties we have attempted to derive information about that shaping process.We have used photometric narrowband observations of a sample of PNe listed in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae to investigate the relationship between PN morphology and the other PN characteristics. The high resolution images were made using ESO's New Technology Telescope and the Hubble Space Telescope. The information we could obtain directly from the observations was augmented by information in the literature in order to address that question. The observations were used to classify the morphologies of 154 PNe, to estimate the sizes of 138 of those nebulae that we considered to lie within the Galactic Bulge, to determine the orientations of 130 of those Bulge nebulae and to derive photometric fluxes for the 69 PNe which had observations of standard stars made during the same night. Information on central star binarity, nebular abundances and radial and expansion velocity was obtained from the literature.Our photometrically derived PNe line fluxes were used to verify 59 H-beta and 69 [OIII] catalogued values (which were obtained using spectroscopy). We found sufficient discrepancy between the values for 9 PNe to merit a further check taking place.We found no distinguishing relationship between PN morphology and any of PN size, radial velocity, or angular location within the Bulge. The abundances of He and O, and the N/O ratio, are generally lower in bipolar nebulae than in those nebulae with no apparent internal structure. We are unable to come to any conclusion as to a relationship between PN morphology and stellar metallicity.Given the short lifespan of PNe and the age of the Bulge it appears that almost all PNe in the Bulge must be associated with low mass stars. The high ratio of bipolar PNe we found in our Bulge sample suggests that, at least within the Bulge, bipolar nebulae are not necessarily associated with high mass stars. Our results show that unlike the orientations of other types of PNe the orientations of the bipolar nebulae in the Bulge are not randomly distributed. Measured to a line tip to tip along the lobes they peak and have their mean approximately along the Galactic Plane. This suggests that the bipolar PNe originate in a different environment from other morphological types, perhaps related to binary separation. However, we find that bipolarity does not imply common-envelope evolution. If the hypothesis that bipolar nebulae are formed in binary star systems is correct, binary systems in the Galactic Bulge have angular momentum vectors that are preferentially aligned along the Galactic Plane. As the orientation appears to be unrelated to lobe size and hence nebular age, the alignment implies that the non-random nature of the angular momentum vectors originated at the time the Bulge stellar population formed. We suggest that it is due to the direction and strength of the ambient magnetic fields.

10

Klus, Helen. "Breaking the quantum limit : the magnetic field of neutron stars in extra-galactic Be X-ray binaries." Thesis, University of Southampton, 2015. https://eprints.soton.ac.uk/381293/.

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Neutron stars are some of the most magnetic objects that have ever been observed, and so they provide physicists with unique environments where fundamental laws of physics can be tested. Neutron stars are typically thought to have magnetic fields between 108 and 1014 G. The effects of the quantum electrodynamics are important above the quantum critical field (BQED) of 4.4×1013 G. In this thesis, I provide evidence that there may be many more neutron stars with B > BQED than previously thought, and that all neutron stars in binary systems that are close to spin equilibrium follow the same relationship between spin period (P) and magnetic field. In Chapter 2, I determine the long-term average X-ray luminosity, spin period, and rate of change of spin period for 42 Be X-ray binaries (BeXB) in the Small Magellanic Cloud (SMC). I use this information, combined with orbital data, to show that the neutron stars in all of these systems are disc-accreting, and that 85% are close to spin equilibrium. All systems with P & 100 s are predicted to have B > BQED. This applies to 2/3 systems. These predicted magnetic fields are higher than those of neutron stars in Galactic BeXB that have had their magnetic fields directly measured via cyclotron resonance scattering features (CRSF). I conclude that this is because the CRSF sources are not close to spin equilibrium. In Chapter 3, I look at pulse-profiles for the neutron stars discussed in Chapter 2 and find that they contain an array of features that vary both across and within individual systems. I suggest that BeXB containing neutron stars with relatively longer spin periods transition from a pencil to a fan beam at lower luminosities. In Chapter 4, I apply the methods used in Chapters 2 and 3 to LXP187, a BeXB in the Large Magellanic Cloud (LMC) that is not close to spin equilibrium. Results for LXP187 help confirm the conclusions of Chapter 2 - that � 2/3 BeXB contain neutron stars with B > BQED.

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Книги з теми "Galactic binaries":

1

NATO Advanced Research Workshop on the Evolution of Galactic X-ray Binaries (1985 Rottach-Egern, Germany). The evolution of galactic X-ray binaries. Dordrecht, Holland: D. Reidel Pub. Co., 1986.

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2

Truemper, J., W. H. G. Lewin, and W. Brinkmann, eds. The Evolution of Galactic X-Ray Binaries. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4594-4.

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3

Kaper, Lex, Edward P. J. van den Heuvel, and Patrick A. Woudt, eds. Black Holes in Binaries and Galactic Nuclei: Diagnostics, Demography and Formation. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/b75143.

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4

North American Workshop on Cataclysmic Variables and Low Mass X-ray Binaries (11th 1989 Santa Fe, N.M.). Accretion-powered compact binaries: Proceedings of the 11th North American Workshop on Cataclysmic Variables and Low Mass X-ray Binaries, Santa Fe, NM, October 9-13, 1989. Cambridge: Cambridge University Press, 1990.

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5

ESLAB Symposium on Two Topics in X-Ray Astronomy (1989 Bologna, Italy). Proceedings of the 23rd ESLAB Symposium on Two Topics in X-Ray Astronomy: Bologna, Italy, 13-20 September 1989. Edited by White N. E. 1952-, Hunt J. J, and Battrick B. 1946-. Paris, France: European Space Agency, 1989.

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6

Truemper, J. The Evolution of Galactic X-Ray Binaries. Springer, 2011.

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7

Dieter, Hils, and United States. National Aeronautics and Space Administration., eds. Confusion noise level due to galactic and extragalactic binaries. [Washington, DC: National Aeronautics and Space Administration, 1997.

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8

(Editor), J. Truemper, W.H.G. Lewin (Editor), and W. Brinkmann (Editor), eds. The Evolution of Galactic X-Ray Binaries (NATO Science Series C:). Springer, 1986.

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9

W, Deutsch Eric, and United States. National Aeronautics and Space Administration., eds. Hubble Space Telescope imaging of bright galactic x-ray binaries in crowded fields. [Washington, DC: National Aeronautics and Space Administration, 1996.

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10

W, Deutsch Eric, and United States. National Aeronautics and Space Administration., eds. Hubble Space Telescope imaging of bright galactic x-ray binaries in crowded fields. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Частини книг з теми "Galactic binaries":

1

Goyal, A. N. "Distribution of Astrometric Binaries in Various Galactic Latitudes." In Astrometric Binaries, 125–31. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5343-7_16.

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2

Lyne, A. G. "A Review of Galactic Millisecond Pulsar Searches." In Compact Stars in Binaries, 225–34. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_18.

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3

Paradijs, Jan. "Galactic Populations Of X-Ray Binaries." In Timing Neutron Stars, 191–207. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_15.

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4

Lu, J. F. "Disk-Driven Precession in Active Close Binaries and in Active Galactic Nuclei." In Active Close Binaries, 239–40. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0679-2_19.

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5

Ritter, H. "Secular Evolution of Cataclysmic Binaries." In The Evolution of Galactic X-Ray Binaries, 271–93. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4594-4_24.

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6

Hellings, P., and C. Loore. "Wind Fed X-Ray Binaries." In The Evolution of Galactic X-Ray Binaries, 51–62. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4594-4_5.

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7

Eggleton, Peter P. "From Wide to Close Binaries ?" In The Evolution of Galactic X-Ray Binaries, 87–105. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4594-4_8.

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8

King, A. R. "Accretion in close binaries." In Galactic High-Energy Astrophysics High-Accuracy Timing and Positional Astronomy, 161–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 1993. http://dx.doi.org/10.1007/3-540-56874-3_4.

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9

Ryan, Sean G. "Element Abundances and Galactic Chemical Evolution." In The Influence of Binaries on Stellar Population Studies, 491–506. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9723-4_35.

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10

Nomoto, Ken’ichi, Keiichi Maeda, Hideyuki Umeda, and Takayoshi Nakamura. "Hypernova Nucleosynthesis and Galactic Chemical Evolution." In The Influence of Binaries on Stellar Population Studies, 507–33. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9723-4_36.

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Тези доповідей конференцій з теми "Galactic binaries":

1

Maccarone, Thomas. "Jets from Galactic Binaries." In The Extreme and Variable High Energy Sky. Trieste, Italy: Sissa Medialab, 2012. http://dx.doi.org/10.22323/1.147.0014.

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2

Jonker, P. G., M. A. P. Torres, D. Steeghs, Reba M. Bandyopadhyay, Stefanie Wachter, Dawn Gelino, and Christopher R. Gelino. "Faint Galactic X-ray Binaries." In A POPULATION EXPLOSION: The Nature & Evolution of X-ray Binaries in Diverse Environments. AIP, 2008. http://dx.doi.org/10.1063/1.2945016.

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3

Zhang, S. N., I. F. Mirabel, B. A. Harmon, R. A. Kroeger, L. F. Rodriguez, R. M. Hjellming, and M. P. Rupen. "Galactic black hole binaries: Multifrequency connections." In The fourth compton symposium. AIP, 1997. http://dx.doi.org/10.1063/1.54121.

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4

Molina, Edgar, Victor A. Acciari, Stefano Ansoldi, Lucio Angelo Antonelli, Axel Arbet Engels, Manuel Artero, Katsuaki Asano, et al. "Recent MAGIC results on Galactic binaries." In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0786.

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5

Nelemans, G. "Galactic Binaries as Sources of Gravitational Waves." In THE ASTROPHYSICS OF GRAVITATIONAL WAVE SOURCES. AIP, 2003. http://dx.doi.org/10.1063/1.1629441.

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6

Grove, J. E., J. E. Grindlay, B. A. Harmon, X. M. Hua, D. Kazanas, and M. McConnell. "Galactic black hole binaries: High-energy radiation." In The fourth compton symposium. AIP, 1997. http://dx.doi.org/10.1063/1.54106.

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7

Dalton, William W., and Craig L. Sarazin. "The galactic high mass x-ray binary population." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45953.

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8

Chiappini, Cristina. "Galactic disk abundance ratios: constraining SNIa stellar yields." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130270.

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9

Calamida, A. "Eclipsing binaries in the galactic globular cluster Omega Centauri." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130216.

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10

White, N. E. "The galactic distribution of black holes in x-ray binaries." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45935.

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