Innermost stable circular orbits in the Majumdar-Papapetrou dihole spacetime

Nakashi, Keisuke; Igata, Takahisa

doi:10.1103/physrevd.99.124033

Cited by 15 publications

(13 citation statements)

References 31 publications

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“…Let us note that as shown in Ref. [33,37] for the 4D MP dihole spacetime, stable circular orbits exist in the asymptotic region for arbitrary separations. Therefore, we can conclude that the appearance of the OSCO is a proper phenomenon of 5D.…”

Section: Summary and Discussionmentioning

confidence: 68%

“…Since this family has singularities on the horizon but not outside it, we can examine the existence of the timelike/null geodesic Killing orbits and their stability throughout the domain of outer communication. The geodesic structure of the 4D MP dihole spacetime has been analyzed in detail in terms of circular/bound orbits and their stability [31][32][33][34][35][36][37][38], chaos [39,40], and shadows [41,42]. The particle dynamics in higher-dimensional MP spacetimes were investigated in Ref.…”

Section: Introductionmentioning

confidence: 99%

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Stable circular orbits in higher-dimensional multi–black-hole spacetimes

Igata¹,

Tomizawa

2020

Phys. Rev. D

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We consider the dynamics of particles, particularly focusing on circular orbits in the higher-dimensional Majumdar-Papapetrou (MP) spacetimes with two equal mass black holes. It is widely known that in the 5D Schwarzschild-Tangherlini and Myers-Perry backgrounds, there are no stable circular orbits. In contrast, we show that in the 5D MP background, stable circular orbits can always exist when the separation of two black holes is large enough. More precisely, for a large separation, stable circular orbits exist from the vicinity of horizons to infinity; for a medium one, they appear only in a certain finite region bounded by the innermost stable circular orbit and the outermost stable circular orbit outside the horizons; for a small one, they do not appear at all. Moreover, we show that in MP spacetimes in more than 5D, they do not exist for any separations.

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Section: Summary and Discussionmentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Stable circular orbits in higher-dimensional multi–black-hole spacetimes

Igata¹,

Tomizawa

2020

Phys. Rev. D

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“…To achieve this, we adopt the Majumdar-Papapetrou (MP) dihole spacetime, which contains two extremal Reissner-Nordström black holes. The circular orbit and its stabilities in the equal mass MP dihole spacetime have been investigated [25][26][27]. In our previous paper [25], we clarified the dependence of the positions of MSCOs and ISCOs on the separation parameter in the equal mass MP * Electronic address: nakashi@rikkyo.ac.jp † Electronic address: igata@rikkyo.ac.jp…”

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confidence: 99%

Effect of a second compact object on stable circular orbits

Nakashi

Igata

2019

Phys. Rev. D

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We investigate how stable circular orbits around a main compact object appear depending on the presence of a second one by using the Majumudar-Papapetrou dihole spacetime, which consists of the two extremal Reissner-Nordström black holes with different masses. While the parameter range of the separation of the two objects is divided due to the appearance of stable circular orbits, this division depends on its mass ratio. We show that the mass ratio range separates into four parts, and we find three critical values as the boundaries. I. INTRODUCTIONRecent progress in the observation of gravitational waves supports the existence of binary black hole systems. The LIGO Scientific and Virgo collaborations have already detected gravitational waves ten times from binary black hole mergers and once from a binary neutron star merger so far [1][2][3][4]. Furthermore, since they have started the third observation run, the number of detections will increase in the future. These results imply that binary black hole systems are a quite common phenomenon in our Universe.A pure binary black hole system is a highly idealized model, around which a third object or matter distribution usually exists in realistic situations. Therefore, one of the next issues is clarifying perturbative interactions with a third body around them. As traditional problems in Newtonian gravity, there are Poincaré's three-body problem and the Kozai mechanism. In recent years, some problems related to these topics have been considered in the framework of the relativistic three body problem [5,6], in the context of resonance in a compound extreme mass ratio inspiral/massive black hole binary [7], and in gravitational wave emission induced by a third body [8][9][10][11]. If a third body itself is the target of observation, we can view it as a test body in a fixed background. As a traditional problem in Newtonian gravity, there is Euler's three-body problem, test particle motion in two fixed centers. The corresponding relativistic system is the main topic of this paper.The study of test body motion is significant for the predictions of astrophysical phenomena around a gravitational system such as a binary. In particular, the circular orbit of a test body plays some essential roles in both theory and observations. In the black hole spacetime, for instance, the bending of light due to strong gravity makes a photon orbit circular near the horizon. If the circular photon orbit is unstable, it relates to the formation of the black hole shadow. On the other hand, the sequence of stable circular massive particle orbits is relevant to accretion disks and a binary system. The innermost stable circular orbit (ISCO) radius is a distinctive one because it is identified as the inner edge of a standard accretion disk model and a compact binary switches the stage of the evolution from the inspiraling phase to the merging phase there [12,13].Actual binary black hole systems exist as highly dynamical systems so that one needs to use the numerical method to analyze the phenomen...

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“…Furthermore, the above expression can be put in Weierstrass form by the transformation: 15) and finally dv dλ 16) and so:…”

Section: Motion In Equatorial Planementioning

confidence: 99%

“…The equilibrium configuration for two extremally rotating BH, or for NS is still an open problem. (12) The study of binary systems have become very important nowadays, since the recent detection of gravitational waves from a binary BH system (13,14,15), and also a binary neutron star system. (16,17) These discoveries establish that binary systems exist in nature, and they strongly motivate the study of the physical properties around these systems.…”

Section: Introductionmentioning

confidence: 99%

Geodesic motion in the Reissner-Nordström space-time

Capobianco¹

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The motion of neutral test particles, both massive and massless, in the space time of a charged source described by the Reissner-Nordström solution is studied. This solution is characterized by two parameters, mass and charge, which defines the horizons of the source. When the mass is larger than the charge, the solution describes a black hole, with two distinct horizons. When the mass and charge are equal there is an extremal black hole, and both horizons merge to one. Finally, when the charge is larger than the mass there is a naked singularity, with no horizon. The structure and properties of these different type of solution are presented and discussed. A general solution of the equations of motion is presented in function of the Weierstrass elliptic function ℘. In addition, the possible orbits for test particles are discussed, and the conditions for existence of closed, circular or escape orbits are presented. The classifications is made based on the particles energy, and the mass and charge of the source. We find that all mentioned orbits are allowed for the three different type of solutions. In particular, for extremal black holes and naked singularities, we find stable circular orbits located outside the event horizon and hence being visible for an external observer.

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Innermost stable circular orbits in the Majumdar-Papapetrou dihole spacetime

Cited by 15 publications

References 31 publications

Stable circular orbits in higher-dimensional multi–black-hole spacetimes

Stable circular orbits in higher-dimensional multi–black-hole spacetimes

Effect of a second compact object on stable circular orbits

Geodesic motion in the Reissner-Nordström space-time

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