Alternative approach to the galactic dark matter problem

Nucamendi, Ulises; Salgado, Marcelo; Sudarsky, Daniel

doi:10.1103/physrevd.63.125016

Cited by 129 publications

(134 citation statements)

References 51 publications

(77 reference statements)

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“…Similar ideas were independently investigated by many authors [23,[26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][40][41][42][43][44][45]. For example, a model with m = 0 was suggested in [27], which has a stability issue.…”

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confidence: 77%

“…Guzman and Matos et al [46,47] extensively studied various astrophysical aspects of the SFDM. Other attempts are based, for example, on a non-minimal coupling [28], quintessence [29,48], Repulsive DM [30], fluid DM [32], nontopological soliton [33], cosh potential [35,36], and ULA [34,37,38] among many [39][40][41][42][43][44]49]. The BEC nature of this DM was extensively studied in [9,23,50] by Harko, Chavanis and their colleagues.…”

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confidence: 99%

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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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Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

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“…As is showed in Refs. [26,27], one can, in principle, model the dark matter in galactic halos with an (inhomogeneous) perfect fluid or scalar fields. For those matter fields T t t = T r r , and therefore N = A −1 , at least in the region where the dark halo is presumably the responsible for the so-called flat rotation curves.…”

Section: Applications and Discussion Of The Theoremmentioning

confidence: 99%

A simple theorem to generate exact black-hole solutions

Salgado

2003

Class. Quantum Grav.

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Under certain conditions imposed on the energy-momentum tensor, a theorem that characterizes a two-parameter family of static and spherically symmetric solutions to Einstein's field equations (black holes), is proved. A discussion on the asymptotics, regularity, and the energy conditions is provided. Examples that include the best known exact solutions within these symmetries are considered. A trivial extension of the theorem includes the cosmological constant ab-initio, providing then a three-parameter family of solutions.

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“…At the early stages of the galactic dark matter model, fully general relativistic stationary solutions were proposed to explain the phenomena like the flatness of rotation curves, assuming the scalar field was real [6,7], non-topological scalar field dark halos [8] complex scalar fields [9] and global monopoles [10]. Later on, the assumptions relaxed to the newtonian limit of such general relativistic models.…”

Section: Introductionmentioning

confidence: 99%

Scalar field dark matter: Head-on interaction between two structures

2006

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In this manuscript we track the evolution of a system consisting of two self-gravitating virialized objects made of a scalar field in the newtonian limit. The Schrödinger-Poisson system contains a potential with self-interaction of the Gross-Pitaevskii type for Bose Condensates. Our results indicate that solitonic behavior is allowed in the scalar field dark matter model when the total energy of the system is positive, that is, the two blobs pass through each other as should happen for solitons; on the other hand, there is a true collision of the two blobs when the total energy is negative.

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Alternative approach to the galactic dark matter problem

Cited by 129 publications

References 51 publications

Brief History of Ultra-light Scalar Dark Matter Models

Brief History of Ultra-light Scalar Dark Matter Models

A simple theorem to generate exact black-hole solutions

Scalar field dark matter: Head-on interaction between two structures

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