Boson Stars: Gravitational Equilibria of Self-Interacting Scalar Fields

Colpi, M.; Shapiro, Stuart L.; Wasserman, Ira

doi:10.1103/physrevlett.57.2485

Cited by 685 publications

(960 citation statements)

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“…In this paper we consider only the case V (Φ) = µ 2 Φ * Φ, where µ is the scalar field mass, without including a scalar self-interaction term. As found in [14] for four dimensional asymptotically flat solutions, although the inclusion of a λ|Φ| 4 term drastically changes the value of the maximum mass and the corresponding critical central density of the boson star solutions, the qualitative features are essentially similar to the non-self interaction case. The Lagrangian density (2) is invariant under a global phase rotation Φ → Φe −iα ; that implies the existence of a conserved current…”

Section: Basic Ansatzsupporting

confidence: 57%

“…For example, boson stars also exhibit a critical mass and critical particle number. Later works considered the more complicated possibilities of the presence of a self interaction for the scalar field [13,14,15] or a nonminimal coupling of the scalar field to gravity [16]. Jetzer and van der Bij extended the model to include a U (1) gauge charge [17] (see also [18]).…”

Section: Introductionmentioning

confidence: 99%

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Boson stars with negative cosmological constant

2003

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We consider boson star solutions in a D-dimensional, asymptotically anti-de Sitter spacetime and investigate the influence of the cosmological term on their properties. We find that for D > 4 the boson star properties are close to those in four dimensions with a vanishing cosmological constant. A different behavior is noticed for the solutions in the three dimensional case. We establish also the non-existence of static, spherically symmetric black holes with a harmonically time-dependent complex scalar field in any dimension greater than two.

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Section: Basic Ansatzsupporting

confidence: 57%

Section: Introductionmentioning

confidence: 99%

Boson stars with negative cosmological constant

2003

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“…The perturbed system of a scalar field with a quartic repulsive interaction but with temperature zero has been studied before [38,28]. The study for the evolution of the SF with the temperature correction in a FRW universe is analogous.…”

Section: Sfdm Density Profiles and Lsb Galaxiesmentioning

confidence: 99%

“…In addition, many numerical simulations have been performed to study the gravitational collapse of the SFDM/BEC model [14,15,28,46,47,48,38,88,89,13]. [24,25] found an approximate analytical expression and numerical solutions of the mass-radius relation of SFDM/BEC halos.…”

Section: Introductionmentioning

confidence: 99%

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

Suárez

Robles

Matos

2013

Astrophysics and Space Science Proceedings

221

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“…Such a boson star is stable by balancing the uncertainty and gravitational pressures. A similar mechanism works in the presence of a quartic self-interaction [22], which dominates over uncertainty pressure, resulting in an equilibrium radius R ≫ 1/m, where m is the boson mass [23]. Hence, we have a universal description of the physics underlying the formation process: once the collapse proceeds far enough, uncertainty, interaction or degeneracy pressure results in a bounce, in which the outgoing shock wave carries away the binding energy.…”

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confidence: 99%

On the formation of degenerate heavy neutrino stars

et al. 2001

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The dynamics of a self-gravitating cold Fermi gas is described using the analogy with an interacting self-gravitating Bose condensate having the same Thomas-Fermi limit. The dissipationless formation of a heavy neutrino star through gravitational collapse and ejection of matter is demonstrated numerically. Such neutrino stars offer an alternative to black holes for the supermassive compact dark objects at the centers of galaxies.Keywords: neutrino stars; boson stars; self-gravitating systems; galactic centers PACS: 02.60. Cb; 95.30.Lz; 95.35.+d; 98.35.Jk Supermassive neutrino stars, in which self-gravity is balanced by the degeneracy pressure of the cold fermions, have been a subject of speculation for more than three decades [1]. Originally, these objects were proposed as models for dark matter in galactic halos and clusters of galaxies, with neutrino masses in the ∼ eV range. More recently, however, degenerate superstars composed of weakly interacting fermions in the ∼ 10 keV range, have been suggested as an alternative to the supermassive black holes that are purported to exist at the centers of galaxies [2][3][4][5][6]. In fact, it has been shown [4] that such degenerate fermion stars could explain the whole range of supermassive compact dark objects which have been observed so far, with masses ranging from 10 6 to 3 × 10 9 M ⊙ , merely assuming that a weakly interacting quasi-stable fermion of mass m f ≃ 15 keV exists in nature.As an example, the most massive compact dark object ever observed, is located at the center of M87, with a mass M ≃ 3.2×10 9 M ⊙ [7]. Interpreting this object as a relativistic fermion star at the Oppenheimer-Volkoff [8] limit, yields a fermion mass of m f ≃ 15 keV and a fermion star radius of R = 4.45R S ≃ 1.5 light-days [3,4], where R S is the Schwarzschild radius. In this case there is little difference between the fermion star and black hole scenarios, because the radius of the last stable orbit around a Schwarzschild black hole is R = 3R S anyway.Extrapolating this down to the compact dark object at the center of our galaxy [9], which, having a mass M ≃ 2.6 × 10 6 M ⊙ , is at the lower limit of the mass range of the observed compact dark objects, we obtain, using the same fermion mass, a radius R ≃ 20 light-days ≃ 5 × 10 4 R S [2]. As the potential inside such a nonrelativistic fermion star is shallow, the spectrum of radiation emitted by accreting baryonic matter is cut off for frequencies larger than 10 13 Hz [3,5], as is actually observed in the spectrum of the enigmatic radio source Sgr A * at the galactic center [10]. A fermion star with radius R < ∼ 20 light-days and mass M ≃ 2.6 × 10 6 M ⊙ is also consistent [6] with the observed motion of stars within a projected distance of 6 to 30 light-days from Sgr A * [9].Of course, it is well-known that 15 keV lies squarely in the cosmologically forbidden mass range for stable active neutrinos ν [11]. The existence of such a massive active neutrino is also disfavoured by the Super-Kamiokande data [12]. However, as shown ...

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Boson Stars: Gravitational Equilibria of Self-Interacting Scalar Fields

Cited by 685 publications

References 10 publications

Boson stars with negative cosmological constant

Boson stars with negative cosmological constant

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

On the formation of degenerate heavy neutrino stars

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