Dark Matter as a Cosmic Bose-Einstein Condensate and Possible Superfluid

Silverman, Mark P.; Mallett, Ronald L.

doi:10.1023/a:1015934027224

Cited by 106 publications

(119 citation statements)

References 12 publications

Supporting

Mentioning

113

Contrasting

Unclassified

Order By: Relevance

“…1. If we solve the differential equation (31) with A 2 > ðA 2 Þ Ã (full lines), the density profile reaches a minimum f min at X ¼ X c before increasing indefinitely. As A 2 approaches ðA 2 Þ Ã from above, the point X c is pushed further and further away while f min decreases.…”

Section: Numerical Solutionmentioning

confidence: 99%

“…On the other hand, some authors [21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36] have proposed that dark matter halos themselves could be in the form of gigantic self-gravitating Bose-Einstein condensates (with or without self-interaction [37]) described by a single wave function c ðr; tÞ. In the Newtonian limit, which is relevant at the galactic scale, the evolution of this wave function is governed by the Gross-Pitaevskii-Poisson (GPP) system [33].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions. II. Numerical results

2011

View full text Add to dashboard Cite

We develop the suggestion that dark matter could be a Bose-Einstein condensate. We determine the mass-radius relation of a Newtonian self-gravitating Bose-Einstein condensate with short-range interactions described by the Gross-Pitaevskii-Poisson system. We numerically solve the equation of hydrostatic equilibrium describing the balance between the gravitational attraction and the pressure due to quantum effects (Heisenberg's uncertainty principle) and short-range interactions (scattering). We connect the noninteracting limit to the Thomas-Fermi limit. We also consider the case of attractive self-interaction. We compare the exact mass-radius relation obtained numerically with the approximate analytical relation obtained with a Gaussian ansatz. An overall good agreement is found.

show abstract

Section: Numerical Solutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions. II. Numerical results

2011

View full text Add to dashboard Cite

show abstract

“…This has lead some to general consideration of Bose-Einstein-Condensate (BEC) dark matter (see, for example, [47][48][49], and in the case of axions [50,51]). Indeed, the numerical simulation of [52] showed that the presence of such an ultra-light scalar condensate indeed reduces the number of dwarf galaxies, but in fact does very little to the cuspy density profile.…”

mentioning

confidence: 99%

Ultralight axions: Degeneracies with massive neutrinos and forecasts for future cosmological observations

et al. 2012

View full text Add to dashboard Cite

A generic prediction of string theory is the existence of many axion fields. It has recently been argued that many of these fields should be light and, like the well known QCD axion, lead to observable cosmological consequences. In this paper we study in detail the effect of the so-called string axiverse on large scale structure, focusing on the morphology and evolution of density perturbations, anisotropies in the cosmic microwave background and weak gravitational lensing of distant galaxies. We quantify specific effects that will arise from the presence of the axionic fields and highlight possible degeneracies that may arise in the presence of massive neutrinos. We take particular care understanding the different physical effects and scales that come into play. We then forecast how the string axiverse may be constrained and show that with a combination of different observations, it should be possible to detect a fraction of ultralight axions to dark matter of a few percent.

show abstract

“…(1) derives from the relation U K = mc 2 1+(p/mc) 2 −1 in which p = /ξ is the fermion linear momentum and ξ = N −1/3 r is the coherence length of the fermion wave function. 5 The second term derives from the magnetic dipole interaction U M = εN µ 2 /ξ 3 simplified to pertain to nearest-neighbor interactions in the two cases in which contiguous moments are either aligned (ε = +1) for minimum entropy or antiparallel (ε = −1) for minimum energy. It will be seen shortly that in a degenerate star, for which the fermions are effectively at 0 K, stable equilibrium results from the parallel alignment of magnetic moments.…”

mentioning

confidence: 99%

Quantum Stabilization of a Relativistic Degenerate Star Beyond the Chandrasekhar Mass Limit

Silverman

2004

Int. J. Mod. Phys. D

Self Cite

View full text Add to dashboard Cite

In contrast to the widely held belief that a degenerate star that has exhausted its nuclear fuel will, if sufficiently massive, unremittingly collapse to a singularity in space (unless the contraction is prevented by some unknown process of quantum gravity acting at the scale of the Planck length), I present a heuristic argument, based on known quantum processes, for the existence of stable equilibrium states of neutron stars and quark stars with macroscopic radii and masses unconstrained by the Chandrasekhar and Oppenheimer-Volkoff limits. The processes that stabilize the star against gravitational contraction involve strong magnetic coupling of the constituent fermions and fermionic pair production at the expense of gravitational potential energy.

show abstract

Dark Matter as a Cosmic Bose-Einstein Condensate and Possible Superfluid

Cited by 106 publications

References 12 publications

Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions. II. Numerical results

Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions. II. Numerical results

Ultralight axions: Degeneracies with massive neutrinos and forecasts for future cosmological observations

Quantum Stabilization of a Relativistic Degenerate Star Beyond the Chandrasekhar Mass Limit

Contact Info

Product

Resources

About