Dark matter interactions with muons in neutron stars

Garani, Raghuveer; Heeck, Julian

doi:10.1103/physrevd.100.035039

Cited by 71 publications

(55 citation statements)

References 90 publications

(146 reference statements)

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“…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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Section: Introductionmentioning

confidence: 99%

Constraints on dark matter from the Moon

Garani

Tinyakov

2020

Physics Letters B

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“…For vector masses above an MeV, the strongest constraints on L μ − L τ range from beam dump experiments, muonic g − 2 measurements, neutrino trident processes, and collider experiments (see, e.g., [28,[33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48]). For lower vector masses, the best published constraints on L μ − L τ arise from ΔN eff through observations of big bang nucleosynthesis [49,50], from SN1987A [51], 2 and neutrino selfinteractions [53][54][55] constraining g 0 ≲ 10 −5 .…”

Section: Introductionmentioning

confidence: 99%

“…NSs with masses of order a solar mass subsequently have 0.15%-0.75% of their mass stored in muons, providing a unique laboratory to test couplings of muons to light new degrees of freedom. This has been leveraged to place constraints on muon-philic dark matter due to its accretion in NSs [45,63,64].…”

Section: Introductionmentioning

confidence: 99%

Probing muonic forces with neutron star binaries

2020

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We show that gravitational wave emission from neutron star binaries can be used to discover any generic long-ranged muonic force due to the large inevitable abundance of muons inside neutron stars. As a minimal consistent example, we focus on a gauged Uð1Þ L μ −L τ symmetry. In pulsar binaries, such Uð1Þ L μ −L τ vectors induce an anomalously fast decay of the orbital period through the emission of dipole radiation. We study a range of different pulsar binaries, finding the most powerful constraints for vector masses below Oð10 −18 eVÞ. For merging binaries, the presence of muons in neutron stars can result in dipole radiation as well as a modification of the chirp mass during the inspiral phase. We make projections for a prospective search using both the GW170817 and S190814bv events and find that current data can discover light vectors with masses below Oð10 −10 eVÞ. In both cases, the limits attainable with neutron stars reach gauge coupling g 0 ≲ 10 −20 , which are many orders of magnitude stronger than previous constraints. We also show projections for next generation experiments, such as Einstein Telescope and Cosmic Explorer.

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“…Here ðQ 1 =m 1 − Q 2 =m 2 Þ ¼ 10 −4 GeV −1 , where Q ¼ N, N is the number of muons which is roughly 10 55 [24]. From Eq.…”

Section: A Psr B1913 + 16: Hulse-taylor Binary Pulsarmentioning

confidence: 99%

“…Besides neutrons, the neutron star contains a lower fraction of electrons, protons, and muons. There are around 10 55 muons compared to about 10 57 neutrons [19][20][21][22][23][24] in a typical old neutron star. The main uncertainties in the following calculations are from the chemical potential and muon content in NS, which should be at most a factor of 2 [24][25][26].…”

Section: Introductionmentioning

confidence: 99%

Vector gauge boson radiation from compact binary systems in a gauged Lμ−Lτ scenario

2019

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The orbital period of a compact binary system decays mainly due to quadrupole gravitational radiation, which agrees with the observation to within 1%. Other types of radiation such as ultralight scalar or pseudoscalar radiation and massive vector boson radiation also contribute to the decay of the orbital period as long as the mass of the emitted particle is less than the orbital frequency of the compact binary system. We obtain an expression of the energy loss due to the radiation of the massive vector field from the neutron star-neutron star and neutron star-white dwarf binaries. Because of the large chemical potential of the degenerate electrons, neutron stars (NSs) have large muon charge. We derive the energy loss due to Uð1Þ L μ −L τ gauge boson radiation from the binaries. For the radiation of the vector boson, the mass is restricted by M Z 0 < Ω ≃ 10 −19 eV, which are the orbital frequencies of the compact star binaries. Using the formula of orbital period decay, we obtain constraints on the coupling constant of the gauge boson in the gauged L μ − L τ theory for the four compact binary systems. For vector gauge boson muon coupling, we find that for M Z 0 < 10 −19 eV, the constraint on the coupling constant is g < Oð10 −20 Þ. We also obtain the exclusion plots of the massive vector Proca field and the gauge field which can couple to muons.

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Dark matter interactions with muons in neutron stars

Cited by 71 publications

References 90 publications

Constraints on dark matter from the Moon

Constraints on dark matter from the Moon

Probing muonic forces with neutron star binaries

Vector gauge boson radiation from compact binary systems in a gauged Lμ−Lτ scenario

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