Stagflation: Bose-Einstein condensation in the early universe

Fukuyama, Takeshi; Morikawa, Masahiro

doi:10.1103/physrevd.80.063520

Cited by 52 publications

(83 citation statements)

References 16 publications

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“…The critical temperature for the condensation to take place is T cr < 2πℎ 2 n 2/3 / mk B (Dalfovo et al 1999). On the other hand, cosmic evolution has the same temperature dependence, since in an adiabatic expansion process the density of a matter‐dominated Universe evolves as ρ∝ T 3/2 (Fukuyama & Morikawa 2009). Therefore, if the boson temperature is equal, for example, to the radiation temperature at z = 1000, the critical temperature for the Bose–Einstein condensation is at present T cr = 0.0027 K (Fukuyama & Morikawa 2009).…”

Section: Cosmological Dynamics Of Bose–einstein Condensatesmentioning

confidence: 99%

Evolution of cosmological perturbations in Bose-Einstein condensate dark matter

Harkó

2011

Monthly Notices of the Royal Astronomical Society

165

131

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We consider the global cosmological evolution and the evolution of the density contrast in the Bose–Einstein condensate dark matter model, in the framework of a post‐Newtonian cosmological approach. In the Bose–Einstein model, dark matter can be described as a non‐relativistic, Newtonian gravitational condensate, whose density and pressure are related by a barotropic equation of state. For a condensate with quartic non‐linearity, the equation of state is polytropic with index n= 1.The basic equation describing the evolution of the perturbations of the Bose–Einstein condensate is obtained, and its solution is studied by using both analytical and numerical methods. The global cosmological evolution as well as the evolution of the perturbations of the condensate dark matter shows significant differences with respect to the pressureless dark matter model, considered in the framework of standard cosmology. Therefore, the presence of condensate dark matter could have modified drastically the cosmological evolution of the early universe as well as the large‐scale structure formation process.

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Section: Cosmological Dynamics Of Bose–einstein Condensatesmentioning

confidence: 99%

Evolution of cosmological perturbations in Bose-Einstein condensate dark matter

Harkó

2011

Monthly Notices of the Royal Astronomical Society

165

131

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“…Nevertheless, by considering some "standard" numerical values, it will be possible to obtain a total qualitative picture of the transition. Consequently, we estimate the values of the dark matter mass and the mean velocity of the non-relativistic dark matter particles, of the order of 1 eV [19,59] and 900 km/s, respectively. According to the general analysis of the condensation process, the first phase of condensation belongs to the standard cold dark matter ( CDM) model.…”

Section: Discussionmentioning

confidence: 99%

“…Based on the above arguments, we assume the possibility that the Bose-Einstein condensation might have happened during the early stages of cosmological evolution of the universe with a temperature comparable to the critical temperature for Bose-Einstein condensation T cr ∼ 2πh 2 n 2/3 /mk B where m is the particle mass, n is the particle density, and k B is Boltzmann's constant [17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32].…”

Section: Introductionmentioning

confidence: 99%

Dark matter as the Bose–Einstein condensation in loop quantum cosmology

Atazadeh¹,

Darabi²,

Mousavi³

2016

Eur. Phys. J. C

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We consider the FLRW universe in a loop quantum cosmological model filled with radiation, baryonic matter (with negligible pressure), dark energy, and dark matter. The dark matter sector is supposed to be of Bose-Einstein condensate type. The Bose-Einstein condensation process in a cosmological context by supposing it as an approximate first-order phase transition, has already been studied in the literature. Here, we study the evolution of the physical quantities related to the early universe description such as the energy density, temperature, and scale factor of the universe, before, during, and after the condensation process. We also consider in detail the evolution era of the universe in a mixed normal-condensate dark matter phase. The behavior and time evolution of the condensate dark matter fraction is also analyzed.

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“…The equilibrium properties of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions were investigated in detail in [35,36]. The study of the cosmological implications of the Bose-Einstein condensation has also become an active field of research [37][38][39][40][41][42][43][44][45][46]. In particular, in [44] it was shown that condensate dark matter effects can be seen in the CMB matter power spectrum if the mass m χ of the condensate particle lies in the range 15 meV < m χ < 700 meV, leading to a small, but perceptible, excess of power at large scales.…”

Section: Introductionmentioning

confidence: 99%

Gravitational, lensing, and stability properties of Bose-Einstein condensate dark matter halos

Harkó

2015

Phys. Rev. D

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The possibility that dark matter, whose existence is inferred from the study of the galactic rotation curves, and from the mass deficit in galaxy clusters, can be in a form of a Bose-Einstein Condensate, has been extensively investigated lately. In the present work, we consider a detailed analysis of the astrophysical properties of the Bose-Einstein Condensate dark matter halos that could provide clear observational signatures that help discriminate between different dark matter models. In the BoseEinstein condensation model dark matter can be described as a non-relativistic, gravitationally confined Newtonian gas, whose density and pressure are related by a polytropic equation of state with index n = 1. The mass and gravitational properties of the condensate halos are obtained in a systematic form, including the mean logarithmic slopes of the density and of the tangential velocity. The lensing properties of the condensate dark matter are investigated in detail. In particular, a general analytical formula for the surface density, an important quantity that defines the lensing properties of a dark matter halos, is obtained in the form of series expansions. This enables arbitraryprecision calculations of the surface mass density, deflection angle, deflection potential, and of the magnification factor, thus giving the possibility of the comparison of the predicted lensing properties of the condensate dark matter halos with observations. The stability properties of the condensate halos are also investigated by using the scalar and the tensor virial theorems, respectively, and the virial perturbation equation for condensate dark matter halos is derived. As an application of the scalar virial theorem we consider the problem of the stability of a slowly rotating and slightly disturbed galactic dark matter halo. For such a halo the oscillations frequencies and the stability conditions are obtained in the linear approximation.

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Stagflation: Bose-Einstein condensation in the early universe

Cited by 52 publications

References 16 publications

Evolution of cosmological perturbations in Bose-Einstein condensate dark matter

Evolution of cosmological perturbations in Bose-Einstein condensate dark matter

Dark matter as the Bose–Einstein condensation in loop quantum cosmology

Gravitational, lensing, and stability properties of Bose-Einstein condensate dark matter halos

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