Minimum mass of galaxies from BEC or scalar field dark matter

Lee, Jae-Weon; Lim, Sooil

doi:10.1088/1475-7516/2010/01/007

Cited by 103 publications

(90 citation statements)

References 63 publications

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“…From this it follows that galaxies can share some properties because they formed in the same manner and at the same moment [67]. Therefore, from this paradigm we have to expect that there exists well formed galaxy halos at higher redshifts than in the ΛCDM model.…”

Section: Why Scalar Field Dark Matter?mentioning

confidence: 91%

“…Robles and Matos [104], (see also [18,16,51]) showed that BEC dark matter halos fit very well high-resolution rotation curves of LSB galaxies, and that the constant density core in dark halos can be reproduced. Also, [67] showed how the SFDM/BEC paradigm is a good alternative to explain the common mass of the dark halos of dwarf spheroidal galaxies. Recently, Rindler-Daller and Shapiro, [103], investigated the formation of vortex in SFDM/BEC halos.…”

Section: Why Scalar Field Dark Matter?mentioning

confidence: 99%

“…Then, the SFDM/BEC model has provided to be a good candidate for dark matter halos of galaxies in the Universe because it can explain many aspects where the standard model of cosmology fails ( [16,18,65,67,64,73,51,104]). Therefore, not only the many successful predictions of the Standard Model of cosmology at large scales are well reproduced by SFDM, but also the ones at galactic scales.…”

Section: Why Scalar Field Dark Matter?mentioning

confidence: 99%

See 2 more Smart Citations

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

Suárez

Robles

Matos

2013

Astrophysics and Space Science Proceedings

231

221

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Section: Why Scalar Field Dark Matter?mentioning

confidence: 91%

Section: Why Scalar Field Dark Matter?mentioning

confidence: 99%

Section: Why Scalar Field Dark Matter?mentioning

confidence: 99%

See 1 more Smart Citation

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

Suárez

Robles

Matos

2013

Astrophysics and Space Science Proceedings

231

221

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“…which leads to the minimum length scale and the mass scale of galactic halos formed at z [62][63][64]. Dwarf galaxies are the smallest dark-matter-dominated objects and, hence, are ideal objects for understanding the nature of dark matter.…”

mentioning

confidence: 99%

Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

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Abstract. This is a review on the brief history of the scalar field dark matter model also known as fuzzy dark matter, BEC dark matter, wave dark matter, or ultra-light axion. In this model ultra-light scalar dark matter particles with mass m = O(10 −22 )eV condense in a single Bose-Einstein condensate state and behave collectively like a classical wave. Galactic dark matter halos can be described as a self-gravitating coherent scalar field configuration called boson stars. At the scale larger than galaxies the dark matter acts like cold dark matter, while below the scale quantum pressure from the uncertainty principle suppresses the smaller structure formation so that it can resolve the small scale crisis of the conventional cold dark matter model.Despite long efforts dark matter (DM) remains a great mystery in physics and astronomy [1]. While numerical results of the cold dark matter (CDM) model are remarkably successful in explaining the large scale structure of the universe, it encounters some problems at the scale of galactic or sub-galactic structures. For example, the numerical simulations usually predict cusped central halo density and too many sub-halos and small galaxies, which seem to be in contradiction with observations [2][3][4][5].Recently, there is a growing interest in the idea that DM particles are ultra-light scalars in Bose-Einstein condensate (BEC). (For a review, see Refs. 6-13) In this model, due to the tiny DM particle mass m = O(10 −22 )eV, the DM particle number density is very high and hence the inter-particle distance is much smaller than the de Broglie wave length of the DM particles. Therefore, the particles are in BEC and move collectively as a wave rather than incoherent particles. At the scale larger than galaxies the DM perturbation behaves like that of CDM, while below the scale quantum pressure from the uncertainty principle suppresses the small structure formation, which makes it a viable alternative to CDM. This property helps us to resolve the small scale problems of the CDM model such as the missing satellite problem or the cusp/core problem [14].Before 2000 there were only a few groups of scientists working on this topic, without much communication even between them. Being unaware of precedent works, many researchers in this field independently proposed similar ideas with various names such as BEC DM, scalar field DM (SFDM), fuzzy DM, ultra-light axion (ULA), ultralight axion like particle (ALP), wave DM, ψ DM, repulsive DM or (super)fluid DM among many, although the basic physics of these models is quite similar. (Henceforth, I will use the term 'SFDM' for the model.) This unfortunate ⋆ e-mail: scikid@jwu.ac.kr situation has brought some confusions among researchers in this field. Therefore, at this point, it is desirable to summarize what have already attempted in this exciting field. 1The hypothesis that galactic DMs are ultra-light scalar particles in BEC has a long history. In Ref.[15] Baldeschi et al. considered the galactic halo model of self-gravitating bosons wit...

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“…The BEC predicts that the size of the galaxies increases as the Hubble radius of the universe even without merging, which agrees well with the recent observational data. In [20] it was shown that the finite length scale of the condensate dark matter can explain the recently observed common central mass of the Milky Way satellites (∼ 10 7 M ⊙ ) independent of their luminosity, if the mass of the dark matter particle is about 10 −22 eV.…”

Section: Introductionmentioning

confidence: 99%

Gravitational collapse of Bose-Einstein condensate dark matter halos

Harkó

2014

Phys. Rev. D

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We study the mechanisms of the gravitational collapse of the Bose-Einstein condensate dark matter halos, described by the zero temperature time-dependent nonlinear Schrödinger equation (the Gross-Pitaevskii equation), with repulsive inter-particle interactions. By using a variational approach, and by choosing an appropriate trial wave function, we reformulate the Gross-Pitaevskii equation with spherical symmetry as Newton's equation of motion for a particle in an effective potential, which is determined by the zero point kinetic energy, the gravitational energy, and the particles interaction energy, respectively. The velocity of the condensate is proportional to the radial distance, with a time dependent proportionality function. The equation of motion of the collapsing dark matter condensate is studied by using both analytical and numerical methods. The collapse of the condensate ends with the formation of a stable configuration, corresponding to the minimum of the effective potential. The radius and the mass of the resulting dark matter object are obtained, as well as the collapse time of the condensate. The numerical values of these global astrophysical quantities, characterizing condensed dark matter systems, strongly depend on the two parameters describing the condensate, the mass of the dark matter particle, and of the scattering length, respectively. The stability of the condensate under small perturbations is also studied, and the oscillations frequency of the halo is obtained. Hence these results show that the gravitational collapse of the condensed dark matter halos can lead to the formation of stable astrophysical systems with both galactic and stellar sizes.

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Minimum mass of galaxies from BEC or scalar field dark matter

Cited by 103 publications

References 63 publications

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

Brief History of Ultra-light Scalar Dark Matter Models

Gravitational collapse of Bose-Einstein condensate dark matter halos

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