Reheating neutron stars with the annihilation of self-interacting dark matter

Chen, Chian-Shu; Lin, Yen-Hsun

doi:10.1007/jhep08(2018)069

Cited by 44 publications

(23 citation statements)

References 102 publications

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“…As borne out by the scaling relation in Eq. (27), the timescales shown would be shorter for smaller neutron stars, and for annihilations dominated by smaller partial wave modes. 3 We limit the plot to radii 13 km since above that radius neutron stars are predicted to have masses M , which are expected to have more massive and larger crusts, invalidating the light-and-thin crust approximation assumed throughout this work.…”

Section: Dark Matter Annihilation Heatingmentioning

confidence: 90%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

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Section: Dark Matter Annihilation Heatingmentioning

confidence: 90%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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show abstract

“…If astrophysical object has no internal heat sources, the heat from the DM annihilations can be detectable in some cases. The DM annihilation in neutron stars [6][7][8][9][10][11][12], in white dwarfs [7,13], in the Earth [14][15][16], and in Mars [17] has been previously considered in this context.…”

Section: Introductionmentioning

confidence: 99%

Constraints on dark matter from the Moon

Garani

Tinyakov

2020

Physics Letters B

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New and complimentary constraints are placed on the spin-independent interactions of dark matter with baryonic matter. Similar to the Earth and other planets, the Moon does not have any major internal heat source. We derive constraints by comparing the rate of energy deposit by dark matter annihilations in the Moon to 12 mW/m 2 as measured by the Apollo mission. For light dark matter of mass O(10) GeV, we also examine the possibility of dark matter annihilations in the Moon limb. In this case, we place constraints by comparing the photon flux from such annihilations to that of the Fermi-LAT measurement of 10 −4 MeV/cm 2 s. This analysis excludes spin independent cross section 10 −37 cm 2 for dark matter mass between 30 and 50 GeV.

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“…Others have calculated the effect of this accumulated dark matter on cooling of celestial objects [34][35][36][37], or have compared the dark luminosity with the observed luminosity to provide stringent constraints on dark matter interactions with SM particles [35,38,39]. More recently, limits on DM-nucleon cross section have also been obtained from non-observation of collapse of massive white dwarfs [40] or from neutron star heating [41][42][43][44].…”

Section: Introductionmentioning

confidence: 99%

Dark matter capture in celestial objects: improved treatment of multiple scattering and updated constraints from white dwarfs

Dasgupta

Gupta

Ray

2019

J. Cosmol. Astropart. Phys.

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We revisit dark matter (DM) capture in celestial objects, including the impact of multiple scattering, and obtain updated constraints on the DM-proton cross section using observations of white dwarfs. Considering a general form for the energy loss distribution in each scattering, we derive an exact formula for the capture probability through multiple scatterings. We estimate the maximum number of scatterings that can take place, in contrast to the number required to bring a dark matter particle to rest. We employ these results to compute a "dark" luminosity L DM , arising solely from the thermalized annihilation products of the captured dark matter. Demanding that L DM not exceed the luminosity of the white dwarfs in the M4 globular cluster, we set a bound on the DM-proton cross section: σ p 10 −44 cm 2 , almost independent of the dark matter mass between 100 GeV and 1 PeV and mildly weakening beyond. This is a stronger constraint than those obtained by direct detection experiments in both large mass (M 5 TeV) and small mass (M 10 GeV) regimes. For dark matter lighter than 350 MeV, which is beyond the sensitivity of present direct detection experiments, this is the strongest available constraint.

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Reheating neutron stars with the annihilation of self-interacting dark matter

Cited by 44 publications

References 102 publications

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Constraints on dark matter from the Moon

Dark matter capture in celestial objects: improved treatment of multiple scattering and updated constraints from white dwarfs

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