Weakly interacting massive particles and neutron stars

Goldman, I.; Nussinov, S.

doi:10.1103/physrevd.40.3221

Cited by 292 publications

(341 citation statements)

References 26 publications

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“…More elaborate calculations were also done by Gould [12,13], taking into account several effects specifically for the case of the Earth and the sun. An estimate of the accretion rate onto a neutron star was also provided by Goldman and Nussinov [16], who were the first to study effects of WIMPs on neutron stars. In this section we calculate the accretion rate of WIMPs onto a typical neu-tron star including also general relativity corrections that turn out to affect the rate up to 70%.…”

Section: Wimp's Accretion Rate Onto the Neutron Starmentioning

confidence: 99%

WIMP annihilation and cooling of neutron stars

2008

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Section: Wimp's Accretion Rate Onto the Neutron Starmentioning

confidence: 99%

WIMP annihilation and cooling of neutron stars

2008

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“…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.…”

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confidence: 99%

“…The third condition necessary for the WIMP collapse into a black hole is the onset of the WIMP selfgravitation. WIMPs captured by the neutron star thermalize within a time t th = 2 × 10 −5 yr (m/GeV) 2 [4,6,9] and concentrate in the center within the radius…”

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confidence: 99%

Excluding Light Asymmetric Bosonic Dark Matter

Kouvaris¹,

Tinyakov²

2011

Phys. Rev. Lett.

177

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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“…In this case, annihilation of trapped weakly interacting massive particles (WIMPs) inside a compact star can produce significant amount of heat that can change the thermal evolution of the star at later times. As a result, stars old enough to be quite cold might maintain higher temperature due to the released heat.The second type of constraints is related to asymmetric dark matter [14,21,[23][24][25][26][27]. In this case WIMPs carry a conserved quantum number and there is an asymmetry between the populations of WIMPs and anti-WIMPs, so that the annihilation is impossible in the present-day universe where only the WIMPs remain.…”

mentioning

confidence: 99%

“…Specifically, compact stars such as white dwarfs and neutron stars have been found to impose severe constraints on some dark matter models [14][15][16][17][18][19][20][21][22][23][24][25][26][27]. In principle, there are two types of effects that can take place in compact stars and can give rise to constraints on dark matter.…”

mentioning

confidence: 99%

(Not)-constraining heavy asymmetric bosonic dark matter

Kouvaris

Tinyakov

2013

Phys. Rev. D

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Recently, constraints on bosonic asymmetric dark matter have been imposed based on the existence of old neutron stars excluding the dark matter masses in the range from ∼ 2 keV up to several GeV. The constraints are based on the star destruction scenario where the dark matter particles captured by the star collapse forming a black hole that eventually consumes the host star. In addition, there were claims in the literature that similar constraints can be obtained for dark matter masses heavier than a few TeV. Here we argue that it is not possible to extend to these constraints. We show that in the case of heavy dark matter, instead of forming a single large black hole that consumes the star, the collapsing dark matter particles form a series of small black holes that evaporate fast without leading to the destruction of the star. Thus, no constraints arise for bosonic asymmetric dark matter particles with masses of a few TeV or higher.Preprint: CP 3 - Origins-2012-034 & DIAS-2012 The last few years stellar observations have been used in order to constrain specific dark matter candidates or predict interesting phenomena related to dark matter [1][2][3][4][5][6][7][8][9][10][11][12][13]. Specifically, compact stars such as white dwarfs and neutron stars have been found to impose severe constraints on some dark matter models [14][15][16][17][18][19][20][21][22][23][24][25][26][27]. In principle, there are two types of effects that can take place in compact stars and can give rise to constraints on dark matter. The first type is related to the thermal evolution of compact stars [15,16,19,20]. In this case, annihilation of trapped weakly interacting massive particles (WIMPs) inside a compact star can produce significant amount of heat that can change the thermal evolution of the star at later times. As a result, stars old enough to be quite cold might maintain higher temperature due to the released heat.The second type of constraints is related to asymmetric dark matter [14,21,[23][24][25][26][27]. In this case WIMPs carry a conserved quantum number and there is an asymmetry between the populations of WIMPs and anti-WIMPs, so that the annihilation is impossible in the present-day universe where only the WIMPs remain. Such kind of WIMPs can accumulate in a compact star quite efficiently as long as the WIMP-nucleon cross section exceeds a certain critical value which in the case of a neutron star is quite small (σ ∼ 10 −46 cm 2 ) [15], several orders of magnitude smaller than current limits from direct searches. Under certain circumstances, the amount of WIMPs accumulated during the lifetime of the star is sufficient to result in a gravitational collapse of the the WIMPs into a black hole. In the case of fermionic * Electronic address: kouvaris@cp3.sdu.dk † Electronic address: Petr.Tiniakov@ulb.ac.be . (1) This amount of WIMPs can be easily accumulated even by nearby known old neutron stars with the standard assumption about dark matter density near the Earth. As it was pointed out in [23], once ∼ 10 36 WIMPs have been ...

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Weakly interacting massive particles and neutron stars

Cited by 292 publications

References 26 publications

WIMP annihilation and cooling of neutron stars

WIMP annihilation and cooling of neutron stars

Excluding Light Asymmetric Bosonic Dark Matter

(Not)-constraining heavy asymmetric bosonic dark matter

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