Gravitational waves from binary black holes as probes of the structure formation history

Nakama, Tomohiro

doi:10.1016/j.dark.2020.100476

Cited by 7 publications

(4 citation statements)

References 48 publications

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“…This would influence the whole analysis in galaxies and may be a direct signature of DM pressure, supporting the hypothesis that DM may not be under the form of dust. 2 Further, a non-vanishing DM pressure clearly produces a dragging effect on test particles that move inside the DM fluid. This is a fair consequence of DM background with a non-zero pressure as this effect happens for nonviscous fluids [38][39][40][41][42].…”

Section: The Dark Matter Equation Of Statementioning

confidence: 97%

“…The first requirement is the presence of super-massive black hole (SMBH) at the center of almost every spiral galaxy [1]. The second is the unavoidable existence of dark matter (DM) halos surrounding every galaxy [2]. In particular, DM existence was originally proposed to explain structure formation and to explain the observed rotational curves (RCs) of stars at the periphery of galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Effects of non-vanishing dark matter pressure in the Milky Way galaxy

Boshkayev,

Konysbayev,

Kurmanov

et al. 2021

Preprint

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We consider the possibility that the Milky Way's dark matter halo possesses a non vanishing equation of state. Consequently, we evaluate the contribution due to the speed of sound, assuming that the dark matter content of the galaxy behaves like a fluid with pressure. In particular, we model the dark matter distribution via an exponential sphere profile in the galactic core, and inner parts of the galaxy whereas we compare the exponential sphere with three widely-used profiles for the halo, i.e. the Einasto, Burkert and Isothermal profile. For the galactic core we also compare the effects due to a dark matter distribution without black hole with the case of a supermassive black hole in vacuum and show that present observations are unable to distinguish them. Finally we investigate the expected experimental signature provided by gravitational lensing due to the presence of dark matter in the core.

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Section: The Dark Matter Equation Of Statementioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Effects of non-vanishing dark matter pressure in the Milky Way galaxy

Boshkayev,

Konysbayev,

Kurmanov

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Recently, the most relevant problems of modern astrophysics and cosmology, such as the problem of the formation of super massive black holes (SMBHs) and the nature of dark matter (DM), have often been debated in the literature [1]. The relevance of the first topic is connected with the latest results of observations of merging black holes (BHs) by the Laser Interferometer Gravitational-Wave Observatory (LIGO) [2,3], observations of the shadow of a black hole in the galaxy M87 using the Event Horizon Telescope (EHT) [4][5][6], and with observations of very distant quasars -one of the brightest objects in the Universe [7], which left almost no doubt about the existence of supermassive black holes.…”

Section: Introductionmentioning

confidence: 99%

Motion of stars near the galactic center

Boshkayev

Konysbayev²,

Kurmanov³

et al. 2021

ijmph

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We investigate the motion of stars at the central region of the Milky Way Galaxy. We consider two possible scenarios: 1) there is a supermassive black hole without dark matter distribution and 2) there is a dark matter core without any black hole in the galactic center. We remark that, with current observations, one cannot distinguish the two separate cases from each other at distances larger than 100 astronomical units. Here, we present improved analyses regarding the motion of stars and show that differences between these two cases appear at distances smaller than 30 astronomical units. We adopt here the so-called exponential density profile for dark matter distribution which is usually used to explain the rotation curve data points in the bulge of galaxies. For simplicity, all computations have been performed within the Newtonian gravity though the effects of general relativity become more pronounced close to the center of the galaxy in the presence of the supermassive black hole without dark matter. We underline our outcomes are model-dependent, i.e. they depend on the choice of the particular dark matter model employed for the analysis.

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“…The possible existence of exotic compact objects is not excluded, as BH candidates alone cannot explain observations, i.e., they are still not able to probe the geometry in proximity astrophysical sources. Remarkable examples are gravitational waves emitted from the inspiral of binary BHs[36], star motion near the galactic center[37], supermassive BH shadows[3], etc 6. Or some sort of DM cloud located at the galactic center, without any super-massive black hole see e.g [39]…”

mentioning

confidence: 99%

Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

D’Agostino¹,

Giambò²,

Luongo³

2022

Preprint

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In this paper, we consider the hypothesis that fractions of dark matter could be constituted by primordial black holes (PBHs). To test this possibility, we work out the observational properties of a static black hole embedded in the dark matter envelope made of a PBH source. The corresponding modifications of geometry due to such a physical system are investigated, with particular focus on the accretion disk luminosity in spiral galaxies. The impact of the PBH presence is analyzed through modification of the disk luminosity and kinematic quantities. Thus, we discuss possible constraints on the PBH abundance in view of the most recent theoretical bounds. The results of our study indicate that suitable PBH masses are MPBH ∈ [10 6 , 10 12 ]M for PBH fractions fPBH ∈ [10 −3 , 1]. In particular, a comparison with the predictions of the exponential sphere density profile for dark matter suggests that the best-matching configuration is achieved for fPBH = 1 and MPBH = 10 6 M . Consequences with respect to the current knowledge on primordial black hole physics are discussed.

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Gravitational waves from binary black holes as probes of the structure formation history

Cited by 7 publications

References 48 publications

Effects of non-vanishing dark matter pressure in the Milky Way galaxy

Effects of non-vanishing dark matter pressure in the Milky Way galaxy

Motion of stars near the galactic center

Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

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