Constraints on Scalar Asymmetric Dark Matter from Black Hole Formation in Neutron Stars

McDermott, Samuel D.; Yu, Hai-Bo; Zurek, Kathryn M.

doi:10.48550/arxiv.1103.5472

Cited by 42 publications

(107 citation statements)

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“…At smaller masses our results are somewhat different because the effect of the Pauli blocking was overestimated in Ref. [27].…”

contrasting

confidence: 75%

“…However, in Ref. [27] the Hawking evaporation of black holes was disregarded which invalidates the constraints for WIMP masses m > 16 GeV. At smaller masses our results are somewhat different because the effect of the Pauli blocking was overestimated in Ref.…”

mentioning

confidence: 75%

“…Note added: When this paper was being finalized Ref. [27] appeared which addressed the same question. However, in Ref.…”

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confidence: 99%

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Excluding Light Asymmetric Bosonic Dark Matter

Kouvaris¹,

Tinyakov²

2011

Phys. Rev. Lett.

172

236

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We argue that current neutron star observations exclude asymmetric bosonic non-interacting dark matter in the range from 2 keV to 16 GeV, including the 5-15 GeV range favored by DAMA and CoGeNT. If bosonic WIMPs are composite of fermions, the same limits apply provided the compositeness scale is higher than ∼ 10 12 GeV (for WIMP mass ∼ 1 GeV). In case of repulsive self-interactions, we exclude large range of WIMP masses and interaction cross sections which complements the constraints imposed by observations of the Bullet Cluster. Apart from direct searches, constraints on WIMPs can be set by observations of compact objects such as white dwarfs and neutron stars [4][5][6][7][8][9][10][11][12]. These constraints can be grouped in two types. The first type targets WIMPs that can annihilate inside the star producing heat that can change the thermal evolution of the star [5]. WIMPs of this type can arise in supersymmetric extensions of the SM (see [13] and references therein), or in Technicolor models [14]. Constraints of the second type target asymmetric DM models. In these models the annihilation of DM in the present-day Universe is impossible because only particles, and no anti-particles (hence the term "asymmetric") remain [15][16][17][18][19]. An additional bonus in these models is that the asymmetry of WIMPs might be linked through sphalerons with the baryon asymmetry [16,18], which can explain the today's ratio Ω DM /Ω B ∼ 5 provided the WIMP has a mass around 5 GeV. Note that this value is not far from the one suggested by DAMA and CoGeNT. In view of this coincidence, the models with WIMP masses in the GeV range have become quite popular.Since in the asymmetric DM models WIMPs cannot annihilate, if a large number of them is accreted during the lifetime of a neutron star, they may collapse forming a small black hole inside the star that eventually destroy the latter. Therefore the existence of old neutron stars can impose constraints on the properties of asymmetric WIMPs. In fact, in the case of fermionic asymmet-

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“…At smaller masses our results are somewhat different because the effect of the Pauli blocking was overestimated in Ref. [27].…”

contrasting

confidence: 75%

mentioning

confidence: 75%

See 1 more Smart Citation

Excluding Light Asymmetric Bosonic Dark Matter

Kouvaris¹,

Tinyakov²

2011

Phys. Rev. Lett.

172

236

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“…Asymmetric dark matter particles captured inside neutron stars and white dwarfs can form a self-gravitating DM cloud which can eventually collapse to a black hole and destroy the star. This argument severely constraints the scattering cross sections of asymmetric dark matter candidates with neutrons [87,88].…”

Section: Multiwavelenght Observations Neutrinos and Other Astrophysic...mentioning

confidence: 99%

Proceedings of the first workshop on Flavor Symmetries and consequences in Accelerators and Cosmology (FLASY2011)

Hirsch¹,

Sierra²,

Leser³

et al. 2012

Preprint

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In this talk I give an overview over continuous and discrete groups and how these are used in the field of model building as flavor symmetries. The latter act on the space of the three generations of elementary particles. I mainly concentrate on discussing generic mathematical properties of these groups relevant for understanding their possible predictive power when applied to explain fermion mass and mixing patterns. I also put emphasis on the classification of discrete groups.13 . Indeed, in all models the leading order result, in this case TB mixing, receives corrections from various sources, e.g. higher-dimensional operators. Thus, in all models a non-zero value of θ l 13 is aspected. Concerning its size one can roughly say: let us assume the size of the corrections to be δ and that the latter contribute in the same manner to all three mixing angles, then the request to not perturb too much the result for the solar mixing angle implies that δ 0.05. Thus, one might expect sin θ l 13 ∼ δ 0.05 which is too small to explain the recent experimental indication. Since in many models several operators give rise to a correction to θ l 13 , we get in general sin θ l 13 ≈ |c|δ with c complex. If c is largish, i.e. the corrections add up, larger values of θ l 13 can be explained. Alternatively, one can consider models in which the corrections to the

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“…Such a phenomenon can be in principle contrasted to observations. The second type of constraints is related to asymmetric dark matter [5][6][7][8][9][10][11][12]. Asymmetric dark matter is an attractive alternative to thermally produced dark matter especially due to the intriguing possibility of relating its asymmetry to the baryonic one.…”

Section: Introductionmentioning

confidence: 99%

The Dark Side of Neutron Stars

Kouvaris

2013

Advances in High Energy Physics

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We review severe constraints on asymmetric bosonic dark matter based on observations of old neutron stars. Under certain conditions, dark matter particles in the form of asymmetric bosonic WIMPs can be effectively trapped onto nearby neutron stars, where they can rapidly thermalize and concentrate in the core of the star. If some conditions are met, the WIMP population can collapse gravitationally and form a black hole that can eventually destroy the star. Based on the existence of old nearby neutron stars, we can exclude certain classes of dark matter candidates.

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Constraints on Scalar Asymmetric Dark Matter from Black Hole Formation in Neutron Stars

Cited by 42 publications

References 0 publications

Excluding Light Asymmetric Bosonic Dark Matter

Excluding Light Asymmetric Bosonic Dark Matter

Proceedings of the first workshop on Flavor Symmetries and consequences in Accelerators and Cosmology (FLASY2011)

The Dark Side of Neutron Stars

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