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Zaremba, E.; Nikuni, Tetsuro; Griffin, Allan

doi:10.1023/a:1021846002995

Cited by 292 publications

(526 citation statements)

References 32 publications

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“…The Heisenberg equation of motion for the quantum field operatorΦ describing the dynamics of a BoseEinstein condensate at arbitrary temperatures is given by [22][23][24][25] i ∂Φ ( r, t) ∂t…”

Section: Finite Temperature Bose-einstein Condensate Dark Mattermentioning

confidence: 99%

“…By introducing the non-condensate field operator ψ ( r, t) so thatΦ ( r, t) = Ψ ( r, t) +ψ ( r, t), where the average value ofψ ( r, t) is zero, ψ ( r, t) = 0, we can separate out the condensate component of the quantum field operator to obtain the equation of motion for Ψ as follows [22][23][24][25] i ∂Ψ ( r, t) ∂t…”

Section: Finite Temperature Bose-einstein Condensate Dark Mattermentioning

confidence: 99%

“…The equilibrium density of the thermal excitations is obtained by integrating the equilibrium Bose -Einstein distribution over the momentum. Thus we obtain [22][23][24][25] …”

Section: Finite Temperature Bose-einstein Condensate Dark Mattermentioning

confidence: 99%

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Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Harkó

Mocanu

2012

Phys. Rev. D

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Once the temperature of a bosonic gas is smaller than the critical, density dependent, transition temperature, a Bose -Einstein Condensation process can take place during the cosmological evolution of the Universe. Bose -Einstein Condensates are very strong candidates for dark matter, since they can solve some major issues in observational astrophysics, like, for example, the galactic core/cusp problem. The presence of the dark matter condensates also drastically affects the cosmic history of the Universe. In the present paper we analyze the effects of the finite dark matter temperature on the cosmological evolution of the Bose-Einstein Condensate dark matter systems. We formulate the basic equations describing the finite temperature condensate, representing a generalized Gross-Pitaevskii equation that takes into account the presence of the thermal cloud in thermodynamic equilibrium with the condensate. The temperature dependent equations of state of the thermal cloud and of the condensate are explicitly obtained in an analytical form. By assuming a flat Friedmann-Robertson-Walker (FRW) geometry, the cosmological evolution of the finite temperature dark matter filled Universe is considered in detail in the framework of a two interacting fluid dark matter model, describing the transition from the initial thermal cloud to the low temperature condensate state. The dynamics of the cosmological parameters during the finite temperature dominated phase of the dark matter evolution are investigated in detail, and it is shown that the presence of the thermal excitations leads to an overall increase in the expansion rate of the Universe.

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Section: Finite Temperature Bose-einstein Condensate Dark Mattermentioning

confidence: 99%

Section: Finite Temperature Bose-einstein Condensate Dark Mattermentioning

confidence: 99%

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Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Harkó

Mocanu

2012

Phys. Rev. D

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“…Our treatment of finite temperatures is based on the ZNG formalism 12 , where we solve the following coupled equations…”

Section: Theorymentioning

confidence: 99%

Matter Wave Solitons at Finite Temperatures

2007

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“…In this vein, microscopic models within the framework of quantum field theory have been proposed [1][2][3][4], as well as mesoscopic (kinetic regime) models employing a generalized version of the Gross-Pitaevskii equation for the superfluid and a quantum Boltzmann equation for the normal fluid [5,6]. The fact that the microscopic quantum field theory does not lead, in the quantum fluids case, to the classical Liouville equation and from there to the classical Boltzmann equation (as it does in classical fluids) has to do with both that (a) the wavelength of the wavefunction associated with the constituent molecules is larger than the interparticle distance, and (b) molecule mobility allows, by enabling particle position interchanges, quantum statistics, i.e., of the effects of particle indistinguishability, to be active (in the quantum fluids case) in all pertinent space-time scales [1].…”

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confidence: 99%

Elementary Vortex Processes in Thermal Superfluid Turbulence

Kivotides

Wilkin

2009

J Low Temp Phys

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By solving pertinent mathematical models with numerical and computational methods, we analyze the formation of superfluid vorticity structures in a turbulent normal fluid with an inertial range exhibiting Kolmogorov scaling. We demonstrate that mutual friction forcing causes quantum vortex instabilities whose signature is spiral vortical configurations. The spirals expand until they accidentally meet metastable, intense normal fluid vorticity tubes of similar curvature and vorticity orientation that trap them by driving them towards low mutual friction sites where superfluid bundles are formed. The bundle formation sites are located within the tube cores, but, due to tube curvature and many-tube interaction effects, are displaced by variable distances from the tube centerlines as they follow the contours of the latter. We analyze possible implications of these processes in fully developed thermal superfluid turbulence dynamics.

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Cited by 292 publications

References 32 publications

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Matter Wave Solitons at Finite Temperatures

Elementary Vortex Processes in Thermal Superfluid Turbulence

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