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

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

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Influence of the initial orbital period and accretion efficiency on the low-mass binary evolution

Serbian Astronomical Journal ◽

10.2298/saj2102025p ◽

2021 ◽

pp. 25-30

Author(s):

J. Petrovic

Keyword(s):

Mass Transfer ◽

Orbital Period ◽

White Dwarf ◽

Binary Systems ◽

Evolutionary Models ◽

Stable Case ◽

Long Period ◽

Low Mass ◽

Orbital Periods ◽

Binary Evolution

This paper presents detailed evolutionary models of low-mass binary systems (1.25 + 1 M?) with initial orbital periods of 10, 50 and 100 days and accretion efficiency of 10%, 20%, 50%, and a conservative assumption. All models are calculated with the MESA (Modules for Experiments in Stellar Astrophysics) evolutionary code. We show that such binary systems can evolve via a stable Case B mass transfer into long period helium white dwarf systems.

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A Dynamical Gravitational Wave Source in a Dense Cluster

Publications of the Astronomical Society of Australia ◽

10.1017/pasa.2016.30 ◽

2016 ◽

Vol 33 ◽

Cited By ~ 20

Author(s):

Jarrod R. Hurley ◽

Anna C. Sippel ◽

Christopher A. Tout ◽

Sverre J. Aarseth

Keyword(s):

Black Holes ◽

Black Hole ◽

Gravitational Wave ◽

Globular Clusters ◽

Binary Systems ◽

Star Cluster ◽

High Density ◽

Wave Source ◽

Black Hole Binaries ◽

Dense Cluster

AbstractMaking use of a new N-body model to describe the evolution of a moderate-size globular cluster, we investigate the characteristics of the population of black holes within such a cluster. This model reaches core-collapse and achieves a peak central density typical of the dense globular clusters of the Milky Way. Within this high-density environment, we see direct confirmation of the merging of two stellar remnant black holes in a dynamically formed binary, a gravitational wave source. We describe how the formation, evolution, and ultimate ejection/destruction of binary systems containing black holes impacts the evolution of the cluster core. Also, through comparison with previous models of lower density, we show that the period distribution of black hole binaries formed through dynamical interactions in this high-density model favours the production of gravitational wave sources. We confirm that the number of black holes remaining in a star cluster at late times and the characteristics of the binary black hole population depend on the nature of the star cluster, critically on the number density of stars and by extension the relaxation timescale.

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GRAVITATIONAL THERMODYNAMICS AND BLACK-HOLE MERGERS

International Journal of Modern Physics A ◽

10.1142/s0217751x00002135 ◽

2000 ◽

Vol 15 (30) ◽

pp. 4871-4875 ◽

Cited By ~ 4

Author(s):

SIMON F. PORTEGIES ZWART ◽

STEPHEN L. W. MCMILLAN

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

Gravitational Waves ◽

Star Clusters ◽

Black Hole Binaries ◽

Orbital Periods ◽

Binary Evolution ◽

Event Rates ◽

Gravitational Thermodynamics

Black holes become the most massive objects early in the evolution of star clusters. Dynamical relaxation then causes them to sink to the cluster core, where they form binaries which become more tightly bound by superelastic encounters with other cluster members. Ultimately, these binaries are ejected from the cluster. The majority of escaping black-hole binaries have orbital periods short enough and eccentricities high enough that the emission of gravitational waves causes them to coalesce within a few billion years. The rate at which such collisions occur is on the order of 10-7 per year per cubic megaparsec. This implies event rates for gravitational-wave detectors substantially greater than current estimates of the corresponding rates from neutron-star mergers or black-hole mergers stemming from pure binary evolution.

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Inventory of black hole binaries

Symposium - International Astronomical Union ◽

10.1017/s0074180900212448 ◽

2003 ◽

Vol 212 ◽

pp. 365-371 ◽

Cited By ~ 6

Author(s):

Jerome A. Orosz

Keyword(s):

Black Holes ◽

Black Hole ◽

Binary Systems ◽

Compact Object ◽

X Rays ◽

Optical Studies ◽

Dynamical Mass ◽

X Ray ◽

Black Hole Binaries ◽

X Ray Binaries

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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Black Holes in General Relativity and Beyond

Proceedings ◽

10.3390/proceedings2019017001 ◽

2019 ◽

Vol 17 (1) ◽

pp. 1 ◽

Cited By ~ 1

Author(s):

Enrico Barausse

Keyword(s):

Black Holes ◽

General Relativity ◽

Black Hole ◽

Gravitational Waves ◽

Physical Interpretation ◽

Binary Systems ◽

Compact Objects ◽

Black Hole Binary ◽

Remarkable Agreement

The recent detections of gravitational waves from binary systems of black holes are in remarkable agreement with the predictions of General Relativity. In this pedagogical mini-review, I go through the physics of the different phases of the evolution of black hole binary systems, providing a qualitative physical interpretation of each one of them. I also briefly describe how these phases would be modified if gravitation were described by a theory extending or deforming General Relativity, or if the binary components turned out to be more exotic compact objects than black holes.

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Black Hole Binaries in Quiescence

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317002083 ◽

2016 ◽

Vol 12 (S324) ◽

pp. 35-38

Author(s):

Charles D. Bailyn

Keyword(s):

Black Hole ◽

Binary Systems ◽

Accretion Rate ◽

Quiescent State ◽

X Ray ◽

Black Hole Binaries ◽

Key Factor ◽

Black Hole Binary ◽

Limiting Case ◽

X Ray Binaries

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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Properties of OB star−black hole systems derived from detailed binary evolution models

Astronomy and Astrophysics ◽

10.1051/0004-6361/201937375 ◽

2020 ◽

Vol 638 ◽

pp. A39 ◽

Cited By ~ 12

Author(s):

N. Langer ◽

C. Schürmann ◽

K. Stoll ◽

P. Marchant ◽

D. J. Lennon ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Radial Velocity ◽

Massive Star ◽

Main Sequence ◽

X Ray ◽

Black Hole Binaries ◽

Star Evolution ◽

Binary Evolution ◽

Massive Star Evolution

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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