The capture of dark matter particles through the evolution of low-mass stars

Lopes, Ilídio; Casanellas, Jordi; Eugénio, Daniel

doi:10.1103/physrevd.83.063521

Cited by 37 publications

(57 citation statements)

References 82 publications

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“…All models are also computed with a local Milky Way orbital velocity v * = 220 km/s which can differ, within the same order of magnitude, for the other two stars. However, that difference introduces only a small error for the capture [35]. clearly evidences that, despite the fact that noannihilation drastically changes DM accumulation, the number of trapped ADM particles is very stiff with respect to the self-capture cross sections.…”

Section: Accumulation Of Self-interacting Asymmetric Dm Inside a mentioning

confidence: 74%

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

2017

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So far, direct detection searches have come empty handed in their quest for Dark Matter (DM). Meanwhile, asteroseismology arises as a complementary tool to study DM, as its accumulation in a star can enhance energy transport, by providing a conduction mechanism, producing significant changes in the stellar structure during the course of the star's evolution. The stellar core, particularly affected by the presence of DM, can be investigated through precise asteroseismic diagnostics. We modelled three stars including DM energy transport: the Sun, a slightly less massive and much older star, KIC 7871531 (0.85 M ⊙ , 9.41 Gyr), and a more massive and younger one, KIC 8379927 (1.12 M ⊙ , 1.82 Gyr). We considered both the case of Weakly Interactive Massive Particles, albeit with a low annihilation, and the case of Asymmetric DM for which the number of trapped particles in the star can be much greater. By analysing these models with asteroseismic separation ratios weighted towards the core, we found indications limiting the effective spin-dependent DM-proton coupling for masses of a few GeV. This independent result is very close to the most recent and most stringent direct detection DM constraints.

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Section: Accumulation Of Self-interacting Asymmetric Dm Inside a mentioning

confidence: 74%

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

2017

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“…The values of σ SI used in the calculation include the values found by the new interpretation of experimental results, comprised of the DAMA/LIBRA and CoGeNT data. If the value of σ SI is larger or equal to σ SD , then the capture of dark matter particles is dominated by the collisions with heavy nuclei, rather than by collisions with hydrogen (Lopes et al 2011).…”

Section: Sun's Evolution In a Non-annihilating Dark Matter Particle Halomentioning

confidence: 99%

“…Alternatively, if the mean free path is large, then the successive collisions are widely separated, so that the energy transfer proceeds within the Knudsen regime . In most of the dark matter scenarios discussed in this paper, the energy transport is dominated by conduction, although, the code has an implementation of the transport of energy by dark matter in both regimes (Lopes et al , 2011.…”

Section: Sun's Evolution In a Non-annihilating Dark Matter Particle Halomentioning

confidence: 99%

“…The stellar code explicitly follows the capture rate of the dark matter particles by the different chemical elements present inside the Sun, some of them changing in isotopic abundance during the Sun's evolution. The paper (Lopes et al 2011) presents a detailed discussion about the properties of dark matter particles, as well as the impact that the uncertainties of the dark matter parameters have on the evolution of the Sun and stars.…”

Section: Sun's Evolution In a Non-annihilating Dark Matter Particle Halomentioning

confidence: 99%

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Solar Neutrino Physics: Sensitivity to Light Dark Matter Particles

Lopes

Silk

2012

ApJ

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Neutrinos are produced in several neutrino nuclear reactions of the proton-proton chain and carbon-nitrogen-oxygen cycle that take place at different radii of the Sun's core. Hence, measurements of solar neutrino fluxes provide a precise determination of the local temperature. The accumulation of non-annihilating light dark matter particles (with masses between 5 GeV and 16 GeV) in the Sun produces a change in the local solar structure, namely, a decrease in the central temperature of a few percent. This variation depends on the properties of the dark matter particles, such as the mass of the particle and its spin-independent scattering cross-section on baryon-nuclei, specifically, the scattering with helium, oxygen, and nitrogen among other heavy elements. This temperature effect can be measured in almost all solar neutrino fluxes. In particular, by comparing the neutrino fluxes generated by stellar models with current observations, namely 8 B neutrino fluxes, we find that non-annihilating dark matter particles with a mass smaller than 10 GeV and a spin-independent scattering cross-section with heavy baryon-nuclei larger than 3 × 10 −37 cm −2 produce a variation in the 8 B neutrino fluxes that would be in conflict with current measurements.

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“…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].…”

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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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The capture of dark matter particles through the evolution of low-mass stars

Cited by 37 publications

References 82 publications

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

Solar Neutrino Physics: Sensitivity to Light Dark Matter Particles

(Not)-constraining heavy asymmetric bosonic dark matter

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