Scalar field dark matter: Head-on interaction between two structures

Bernal, Argelia; Guzmán, F. S.

doi:10.1103/physrevd.74.103002

Cited by 92 publications

(114 citation statements)

References 28 publications

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“…The spherical derivatives in (52) and (53) are approximated by center finite difference. In the spherical shell two patches share a common radial coordinate and adjacent patches share the angular coordinate perpendicular to the mutual boundary.…”

Section: A Numerical Methodsmentioning

confidence: 99%

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Binary black hole mergers inf(R)theory

2013

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In the near future, gravitational wave detection is set to become an important observational tool for astrophysics. It will provide us with an excellent means to distinguish different gravitational theories. In effective form, many gravitational theories can be cast into an f (R) theory. In this article, we study the dynamics and gravitational waveform of an equal-mass binary black hole system in f (R) theory. We reduce the equations of motion in f (R) theory to the Einstein-Klein-Gordon coupled equations. In this form, it is straightforward to modify our existing numerical relativistic codes to simulate binary black hole mergers in f (R) theory. We considered binary black holes surrounded by a shell of scalar field. We solve the initial data numerically using the Olliptic code. The evolution part is calculated using the extended AMSS-NCKU code. Both codes were updated and tested to solve the problem of binary black holes in f (R) theory. Our results show that the binary black hole dynamics in f (R) theory is more complex than in general relativity. In particular, the trajectory and merger time are strongly affected. Via the gravitational wave, it is possible to constrain the quadratic part parameter of f (R) theory in the range |a2| < 10 11 m 2 . In principle, a gravitational wave detector can distinguish between a merger of binary black hole in f (R) theory and the respective merger in general relativity. Moreover, it is possible to use gravitational wave detection to distinguish between f (R) theory and a non self-interacting scalar field model in general relativity.

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Section: A Numerical Methodsmentioning

confidence: 99%

“…Astrophysical models often include EKG equations for the description of certain phenomena. For example, there are models of dark matter which use EKG in the weak field limit [50][51][52][53]. One example of relativistic scalar field is boson stars [54][55][56][57][58].…”

Section: Dynamics Of the Binary Black Hole Induced By The Scalar Fieldmentioning

confidence: 99%

Binary black hole mergers inf(R)theory

2013

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“…These are called boson stars for complex scalar fields (Ruffini & Bonazzola 1969;Lee & Koh 1996;Guzmán 2006), and oscillations for real scalar fields (Seidel & Suen 1991;Ureña-López 2002;Alcubierre et al 2003). There are also scalar field stable gravitational structures described by the Schrödinger-Poisson system , 2006Bernal & Guzmán 2006). One of the most promising and physically interesting features of SFDM resides on the hypothesis that it describes cosmological Bose-Einstein condensates (BEC; see, for example, Woo & Chiueh 2009;Ureña 2009).…”

Section: Introductionmentioning

confidence: 99%

Ultra Light Bosonic Dark Matter and Cosmic Microwave Background

Rodríguez‐Montoya

Magaña

Matos

et al. 2010

ApJ

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In this paper, we consider the hypothesis in which a species of ultra light bosonic dark matter (ULBDM) with mass m B ∼ 10 −22 eV could be the dominant dark matter (DM) in the universe. As a first approach we work in the context of kinetic theory, where ULBDM is described by the phase space distribution function whose dynamics is dictated by the Boltzmann-Einstein equations. We investigate the effects that this kind of DM imprints in the acoustic peaks of the cosmic microwave background. We find that the effect of the Bose-Einstein statistics is small, albeit perceptible, and is equivalent to an increase of nonrelativistic matter. It is stressed that in this approach, the mass-to-temperature ratio necessary for ULBDM to be a plausible DM candidate is about five orders of magnitude. We show that reionization is also necessary and we address a range of consistent values for this model. We find that the temperature of ULBDM is below the critical value implying that Bose-Einstein condensation is inherent to the ULBDM paradigm.

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“…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%