Static configurations of dark energy and dark matter

Brouzakis, N.; Tetradis, N.

doi:10.1088/1475-7516/2006/01/004

Cited by 33 publications

(32 citation statements)

References 41 publications

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“…In particular, it was used in studying compact objects in Refs. [24,29,30], in describing structure formation in Ref. [31], and in modeling interacting DM and DE in the papers [14,19].…”

Section: Equations For Equilibrium Configurationsmentioning

confidence: 99%

“…[2,20]) have a number of interesting features and may be used in solving some known problems of modern cosmology, for example, the so-called coincidence problem. In turn, the supposed presence in the Universe of DE, in one form or another, and DM provides the basis for concluding that compact systems consisting of dark energy [21], of dark matter [22,23], or of interacting DE and DM [24,25] might also exist.…”

Section: Introductionmentioning

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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“…In particular, it was used in studying compact objects in Refs. [24,29,30], in describing structure formation in Ref. [31], and in modeling interacting DM and DE in the papers [14,19].…”

Section: Equations For Equilibrium Configurationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Chameleon dark matter stars

2013

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“…Following [31], we use the Thomas-Fermi approximation to describe the distribution of the dark matter particles assuming weak interaction and no scattering. Then dark matter particles at every point of space-time having local Fermi momentum p(r) obey the distribution…”

Section: B Particle Physics Ingredientsmentioning

confidence: 99%

Static structure of chameleon dark matter as an explanation of dwarf spheroidal galaxy cores

Chanda¹,

Das²

2017

Phys. Rev. D

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We propose a novel mechanism that explains the cored dark matter density profile in recently observed dark matter rich dwarf spheroidal galaxies. In our scenario, dark matter particle mass decreases gradually as a function of distance towards the center of a dwarf galaxy due to its interaction with a chameleon scalar. At closer distance towards the Galactic center the strength of attractive scalar fifth force becomes much stronger than gravity and is balanced by the Fermi pressure of the dark matter cloud; thus, an equilibrium static configuration of the dark matter halo is obtained. Like the case of soliton star or fermion Q-star, the stability of the dark matter halo is obtained as the scalar achieves a static profile and reaches an asymptotic value away from the Galactic center. For simple scalar-dark matter interaction and quadratic scalar self-interaction potential, we show that dark matter behaves exactly like cold dark matter (CDM) beyond a few kpc away from the Galactic center but at closer distance it becomes lighter and Fermi pressure cannot be ignored anymore. Using Thomas-Fermi approximation, we numerically solve the radial static profile of the scalar field, fermion mass and dark matter energy density as a function of distance. We find that for fifth force mediated by an ultralight scalar, it is possible to obtain a flattened dark matter density profile towards the Galactic center. In our scenario, the fifth force can be neglected at distance r ≥ 1 kpc from the Galactic center and dark matter can be simply treated as heavy nonrelativistic particles beyond this distance, thus reproducing the success of CDM at large scales.

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“…[43]). However, one can use instead a phenomenological possibility when a description of the interaction between the scalar field and matter is performed assuming that the pressure and density are not initially explicit functions of a scalar field.…”

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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Static configurations of dark energy and dark matter

Cited by 33 publications

References 41 publications

Chameleon dark matter stars

Chameleon dark matter stars

Static structure of chameleon dark matter as an explanation of dwarf spheroidal galaxy cores

Wormhole solutions supported by interacting dark matter and dark energy

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