Chameleon stars

Dzhunushaliev, Vladimir; Folomeev, Vladimir; Singleton, Douglas

doi:10.1103/physrevd.84.084025

Cited by 40 publications

(106 citation statements)

References 39 publications

(105 reference statements)

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“…The existence of slowly rotating fermion-boson stars was shown in [65], although no solutions were found in previous attempts [136]. Also see [73] for unstable solutions consisting of a real scalar field coupled to a perfect fluid with a polytropic equation of state.…”

Section: Varieties Of Boson Starsmentioning

confidence: 99%

Dynamical Boson Stars

Liebling

Palenzuela

2012

Living Rev. Relativ.

521

547

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The idea of stable, localized bundles of energy has strong appeal as a model for particles. In the 1950s, John Wheeler envisioned such bundles as smooth configurations of electromagnetic energy that he called geons, but none were found. Instead, particle-like solutions were found in the late 1960s with the addition of a scalar field, and these were given the name boson stars. Since then, boson stars find use in a wide variety of models as sources of dark matter, as black hole mimickers, in simple models of binary systems, and as a tool in finding black holes in higher dimensions with only a single Killing vector. We discuss important varieties of boson stars, their dynamic properties, and some of their uses, concentrating on recent efforts.

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Section: Varieties Of Boson Starsmentioning

confidence: 99%

Dynamical Boson Stars

Liebling

Palenzuela

2012

Living Rev. Relativ.

521

547

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“…In the cosmological context, the Lagrangian (1) was used in modeling the present accelerated expansion of the Universe [15,[32][33][34][35][36], in describing structure formation [37], and when considering compact configurations [36,38]. In doing so, a choice of the Lagrangian L m is, in general, not unique.…”

Section: Equations For Equilibrium Configurationsmentioning

confidence: 99%

“…However, it can be shown that, for instance, for static configurations, these Lagrangians, being substituted in the general Lagrangian (1), will give different equations for an equilibrium configuration [the Tolman-Oppenheimer-Volkoff (TOV) equations]. In the case of L m ¼ p, the TOV equation will have the same form as when f ¼ 1 [36,38]. On the other hand, the use of L m ¼ À" leads to the appearance of an extra term on the right-hand side of the TOV equation associated with the nonminimal coupling [see Eq.…”

Section: Equations For Equilibrium Configurationsmentioning

confidence: 99%

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Chameleon dark matter stars

2013

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We consider static, spherically symmetric equilibrium configurations consisting of fermionic dark matter nonminimally coupled to dark energy in the form of a quintessence scalar field. With the scalar field coupling function, the form of which is taken to meet cosmological observations, we estimate the effect of such a nonminimal coupling on the properties of dark matter compact configurations. We show that the masses and sizes of the resulting chameleon dark matter stars are smaller than those of systems with no field present.Comment: 10 pages, 2 figures, Introduction revised, Conclusion extended, choice of the interaction Lagrangian discussed in detail, some other minor corrections to content, new references added, version published in PRD. arXiv admin note: text overlap with arXiv:1308.320

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“…The case f → 1 corresponds to the absence of a direct coupling between matter and the scalar field, when the two sources are coupled only via gravity. In the cosmological context, the interaction Lagrangian (1) was used in modeling the present accelerated expansion of the Universe [34,[49][50][51][52][53], in describing structure formation [54], and when considering compact configurations [53,55]. In doing so, a choice of the Lagrangian L m is, in general, not unique.…”

Section: Derivation Of the Equations For Equilibrium Configurationsmentioning

confidence: 99%

Wormhole solutions supported by interacting dark matter and dark energy

Folomeev

Dzhunushaliev

2014

Phys. Rev. D

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We show that the presence of a nonminimal interaction between dark matter and dark energy may lead to a violation of the null energy condition and to the formation of a configuration with nontrivial topology (a wormhole). In this it is assumed that both dark matter and dark energy satisfy the null energy condition, a violation of which takes place only in the inner high-density regions of the configuration. This is achieved by assuming that, in a high-density environment, a nonminimal coupling function changes its sign in comparison with the case where dark matter and dark energy have relatively low densities which are typical for a cosmological background. For this case, we find regular static, spherically symmetric solutions describing wormholes supported by dark matter nonminimally coupled to dark energy in the form of a quintessence scalar field.

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Chameleon stars

Cited by 40 publications

References 39 publications

Dynamical Boson Stars

Dynamical Boson Stars

Chameleon dark matter stars

Wormhole solutions supported by interacting dark matter and dark energy

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