Boson stars from self-interacting dark matter

Eby, Joshua; Kouvaris, Chris; Nielsen, Niklas Grønlund; Wijewardhana, L. C. R.

doi:10.1007/jhep02(2016)028

Cited by 136 publications

(128 citation statements)

References 137 publications

Supporting

Mentioning

124

Contrasting

Order By: Relevance

“…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.…”

mentioning

confidence: 68%

Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

View full text Add to dashboard Cite

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...

show abstract

mentioning

confidence: 68%

Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

View full text Add to dashboard Cite

show abstract

“…The author found that, as its potential is unbounded from below, a star of this kind collapses all the way to its Schwarzschild radius and forms a black hole. Indeed, the leading axion self-interaction is attractive; axionic or other bosonic objects with repulsive interactions have been considered by [30,31]. However, the axion potential contains additional terms which become increasingly important as the axion density becomes large.…”

Section: Introductionmentioning

confidence: 99%

Collapse of axion stars

Eby

Leembruggen

Surányi

et al. 2016

J. High Energ. Phys.

Self Cite

109

191

View full text Add to dashboard Cite

Axion stars, gravitationally bound states of low-energy axion particles, have a maximum mass allowed by gravitational stability. Weakly bound states obtaining this maximum mass have sufficiently large radii such that they are dilute, and as a result, they are well described by a leading-order expansion of the axion potential. Heavier states are susceptible to gravitational collapse. Inclusion of higher-order interactions, present in the full potential, can give qualitatively different results in the analysis of collapsing heavy states, as compared to the leading-order expansion. In this work, we find that collapsing axion stars are stabilized by repulsive interactions present in the full potential, providing evidence that such objects do not form black holes. In the last moments of collapse, the binding energy of the axion star grows rapidly, and we provide evidence that a large amount of its energy is lost through rapid emission of relativistic axions.

show abstract

“…In that paper, we showed that one could find approximate solutions to these equations, by using a combination of analytical and numerical methods. We showed that our methods were numerically stable, and that they converged uniformly far away from the core of the star, and furthermore were much less computationally expensive compared to other purely numerical methods [18,[22][23][24][25][26][27][28][29][30][31][32][33][34][35].…”

Section: Introductionmentioning

confidence: 80%

Profiles of boson stars with self-interactions

Kling

Rajaraman

2018

Phys. Rev. D

View full text Add to dashboard Cite

Under the influence of gravity, light scalar fields can form bound compact objects called boson stars. We use the semianalytic approach of matching asymptotic expansions to obtain the profile for boson stars where the constituent particles have self-interactions. We obtain parametric representations of these profiles as a function of the self-interactions, including the case of very strong self-interactions. We show that our methods agree with solutions obtained by purely numerical methods. Significant distortions are found as compared to the noninteracting case.

show abstract

Boson stars from self-interacting dark matter

Cited by 136 publications

References 137 publications

Brief History of Ultra-light Scalar Dark Matter Models

Brief History of Ultra-light Scalar Dark Matter Models

Collapse of axion stars

Profiles of boson stars with self-interactions

Contact Info

Product

Resources

About