Boson stars in biscalar extensions of Horndeski gravity

Brihaye, Yves; Cisterna, Adolfo; Erices, Cristián

doi:10.1103/physrevd.93.124057

Cited by 84 publications

(54 citation statements)

References 104 publications

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“…The e = 0 case was studied in Ref. [17]. Note that the line for the β < 0 solutions is the line of end points for any value of e: the maximal f (0) depends on β but not on e.…”

Section: Solutions and Their Propertiesmentioning

confidence: 99%

“…Quite recently, black hole solutions [12,13,14,15] were discovered in this "John"-type version of Horndeski theory. Black hole solutions [16] were found also in a "biscalar extension" of the theory and boson stars were found [17] in a different biscalar version where the scalar field becomes complex. On the other hand, the real scalar system was also studied in the presence of a radial electric field [18,19] and black holes were found in that case too.…”

Section: Introductionmentioning

confidence: 99%

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Charged boson stars and black holes with nonminimal coupling to gravity

Verbin

Brihaye

2018

Phys. Rev. D

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We find new spherically symmetric charged boson star solutions of a complex scalar field coupled nonminimally to gravity by a "John-type" term of Horndeski theory, that is a coupling between the kinetic scalar term and Einstein tensor. We study the parameter space of the solutions and find two distinct families according to their position in parameter space. More widespread is the family of solutions (which we call branch 1) existing for a finite interval of the central value of the scalar field starting from zero and ending at some finite maximal value. This branch contains as a special case the charged boson stars of the minimally coupled theory. In some regions of parameter space we find a new second branch ("branch 2") of solutions which are more massive and more stable than those of branch 1. This second branch exists also in a finite interval of the central value of the scalar field, but its end points (either both or in some cases only one) are extremal Reissner-Nordström black hole solutions.

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“…The e = 0 case was studied in Ref. [17]. Note that the line for the β < 0 solutions is the line of end points for any value of e: the maximal f (0) depends on β but not on e.…”

Section: Solutions and Their Propertiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Charged boson stars and black holes with nonminimal coupling to gravity

Verbin

Brihaye

2018

Phys. Rev. D

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“…(32), (38) and (39) and Φ ′ (0) = −5.7 × 10 −16 cm −1 in the central density interval considered. In order to compare the structure of the stars in hybrid metric-Palatini gravity and standard general relativity we also present the mass-radius relation for stiff fluid stars, obtained as the solutions of the general relativistic mass continuity and TOV equations (55) and (56), respectively.…”

Section: Stiff Fluid Starsmentioning

confidence: 99%

“…Besides the information of the maximum masses and radii of neutron or other stars, observations of the surface gravitational redshift can also provide important constraints on modified theories of gravity. The structure and physical properties of specific classes of neutron, quark and exotic stars in various modified gravity theories have been extensively studied in [45][46][47][48][49][50][51][52][53][54][55][56].…”

Section: Introductionmentioning

confidence: 99%

Hybrid metric-Palatini stars

et al. 2017

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We consider the internal structure and the physical properties of specific classes of neutron, quark and Bose-Einstein Condensate stars in the recently proposed hybrid metric-Palatini gravity theory, which is a combination of the metric and Palatini f (R) formalisms. It turns out that the theory is very successful in accounting for the observed phenomenology, since it unifies local constraints at the Solar System level and the late-time cosmic acceleration, even if the scalar field is very light. In this paper, we derive the equilibrium equations for a spherically symmetric configuration (mass continuity and Tolman-Oppenheimer-Volkoff) in the framework of the scalar-tensor representation of the hybrid metric-Palatini theory, and we investigate their solutions numerically for different equations of state of neutron and quark matter, by adopting for the scalar field potential a Higgstype form. It turns out that the scalar-tensor definition of the potential can be represented as an Clairaut differential equation, and provides an explicit form for f (R) given by f (R) ∼ R + Λ eff , where Λ eff is an effective cosmological constant. Furthermore, stellar models, described by the stiff fluid, radiation-like, the bag model and the Bose-Einstein Condensate equations of state are explicitly constructed in both General Relativity and hybrid metric-Palatini gravity, thus allowing an in-depth comparison between the predictions of these two gravitational theories. As a general result it turns out that for all the considered equations of state, hybrid gravity stars are more massive than their general relativistic counterparts. Furthermore, two classes of stellar models corresponding to two particular choices of the functional form of the scalar field (constant value, and logarithmic form, respectively), are also investigated. Interestingly enough, in the case of a constant scalar field the equation of state of the matter takes the form of the bag model equation of state describing quark matter. As a possible astrophysical application of the obtained results we suggest that stellar mass black holes, with masses in the range of 3.8M⊙ and 6M⊙, respectively, could be in fact hybrid metric-Palatini gravity neutron or quark stars.

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“…In addition, solutions describing neutron stars and other compact objects have come out, imposing several constraints on the validity of these kinds of models [28][29][30][31]. These theories attracted a lot of interest also in the cosmology community as they might play a role in explaining inflation, dark energy, or dark matter [32].…”

Section: Introductionmentioning

confidence: 99%

Static and rotating solutions for vector-Galileon theories

et al. 2016

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We consider a particular truncation of the generalized Proca field theory in four dimensions for which we construct static and axisymmetric rotating black hole "stealth solutions," namely solutions with (anti) de Sitter or Kerr metric but nontrivial vector field. The static configuration is promoted to a backreacting black hole with asymptotic (anti) de Sitter behavior by turning on a nonlinear electrodynamic source given as a fixed power of the Maxwell invariant. Finally we extend our solutions to arbitrary dimensions.

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Boson stars in biscalar extensions of Horndeski gravity

Cited by 84 publications

References 104 publications

Charged boson stars and black holes with nonminimal coupling to gravity

Charged boson stars and black holes with nonminimal coupling to gravity

Hybrid metric-Palatini stars

Static and rotating solutions for vector-Galileon theories

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