Mini-soliton stars

Friedberg, R.; Lee, T. D.; Pang, Y.

doi:10.1103/physrevd.35.3640

Cited by 247 publications

(287 citation statements)

References 3 publications

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“…which can be derived from the EKG for weak gravity [53] using ψ = √ mϕ or from the many-body formalism. Here, the DM density is ρ d = m|ψ| 2 = m 2 |ϕ| 2 and V is the self-gravitation potential.…”

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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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confidence: 99%

Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

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“…2.28-2.30. We find that: 14) establishing in this way the frequency as a measure of the gravity strength.…”

Section: Q-stars With Two Scalar Fieldsmentioning

confidence: 96%

“…Einstein equations read, dropping the tildes and the O(ǫ) terms: 12) and the Lagrange equations are: 14) with initial conditions A(0) = 1, B(∞) = 1 and A ′ 0 (0) = 0. The other initial condition for the value of the gauge field can be received by repeating the discussion referring to the surface, because the frequency ω is now replaced by the dynamical variable θ.…”

Section: Scalar-fermion Q-starsmentioning

confidence: 99%

Q-Stars in Anti de Sitter Spacetime

Prikas

2004

General Relativity and Gravitation

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“…However, it is evident that for a large enough mass scale, gravitational effects become important and one needs to study Q-stars [20,21,22]. The existence of Q-stars was demonstrated by Friedberg et al [23] and by Lynn [24]. Further studies revealed more features like the fact that gravity limits the size of Q-balls [25] or the properties of spinning Q-stars [16], or made generalizations like Q-stars with non-minimal coupling to gravity [26].…”

Section: Introductionmentioning

confidence: 99%

Sigma modelQ-balls andQ-stars

Verbin

2007

Phys. Rev. D

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A new kind of Q-balls is found: Q-balls in a non-linear sigma model. Their main properties are presented together with those of their self-gravitating generalization, sigma model Q-stars. A simple special limit of solutions which are bound by gravity alone ("sigma stars") is also discussed briefly. The analysis is based on calculating the mass, global U(1) charge and binding energy for families of solutions parameterized by the central value of the scalar field. Two kinds (differing by the potential term) of the new sigma model Q-balls and Q-stars are analyzed. They are found to share some characteristics while differing in other respects like their properties for weak central scalar fields which depend strongly on the form of the potential term. They are also compared with their "ordinary" counterparts and although similar in some respects, significant differences are found like the existence of an upper bound on the central scalar field. The sigma model Q-stars also contain non-solitonic solutions whose relation with sigma star solutions is discussed.

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Mini-soliton stars

Cited by 247 publications

References 3 publications

Brief History of Ultra-light Scalar Dark Matter Models

Brief History of Ultra-light Scalar Dark Matter Models

Q-Stars in Anti de Sitter Spacetime

Sigma modelQ-balls andQ-stars

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