Direct detection of bound states of asymmetric dark matter

Coskuner, Ahmet; Grabowska, Dorota; Knapen, Simon; Zurek, Kathryn M.

doi:10.1103/physrevd.100.035025

Cited by 51 publications

(59 citation statements)

References 103 publications

(188 reference statements)

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“…Another mechanism for achieving a larger characteristic interaction radius is dark matter that is not a point particle but instead has a finite physical extent [90,[110][111][112][113][114][115][116][117][118][119][120][121][122][123][124]. Such dark matter could take the form of a composite particle.…”

Section: Composite Dark Mattermentioning

confidence: 99%

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

et al. 2019

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Critical probes of dark matter come from tests of its elastic scattering with nuclei. The results are typically assumed to be model independent, meaning that the form of the potential need not be specified and that the cross sections on different nuclear targets can be simply related to the cross section on nucleons. For pointlike spin-independent scattering, the assumed scaling relation is σ χA ∝ A 2 μ 2 A σ χN ∝ A 4 σ χN , where the A 2 comes from coherence and the μ 2 A ≃ A 2 m 2 N from kinematics for m χ ≫ m A. Here we calculate where model independence ends, i.e., where the cross section becomes so large that it violates its defining assumptions. We show that the assumed scaling relations generically fail for dark matter-nucleus cross sections σ χA ∼ 10 −32-10 −27 cm 2 , significantly below the geometric sizes of nuclei and well within the regime probed by underground detectors. Last, we show on theoretical grounds, and in light of existing limits on light mediators, that pointlike dark matter cannot have σ χN ≳ 10 −25 cm 2 , above which many claimed constraints originate from cosmology and astrophysics. The most viable way to have such large cross sections is composite dark matter, which introduces significant additional model dependence through the choice of form factor. All prior limits on dark matter with cross sections σ χN > 10 −32 cm 2 with m χ ≳ 1 GeV must therefore be reevaluated and reinterpreted.

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Section: Composite Dark Mattermentioning

confidence: 99%

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

et al. 2019

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“…At larger cross sections, the implied DMnucleus cross section is larger than the physical area of nuclei, implying either long-range forces (e.g. mediation by light dark photons [13,33]) or composite dark matter [34].…”

Section: Dark Matter Capturementioning

confidence: 98%

Terrestrial and martian heat flow limits on dark matter

et al. 2020

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If dark matter is efficiently captured by a planet, energy released in its annihilation can exceed that planet's total heat output. Building on prior work, we treat Earth's composition and dark matter capture in detail and present improved limits on dark matter-nucleon scattering cross sections for dark matter masses ranging from 0.1 to 10 10 GeV. We also extend Earth limits by applying the same treatment to Mars. The scope of dark matter models considered is expanded to include spin-dependent nuclear interactions including isospin-independent, proton only, and neutron only interactions. We find that Earth and Mars heating bounds are alleviated for dark matter s-wave self-annihilation cross sections 10 −37 cm 2 .

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“…color-charged dark matter [78][79][80], near-Planck mass dark matter [81], monopole dark matter (e.g. [82]), and dark matter composed of many constituent states, also known as composite dark matter [83][84][85][86][87][88][89].…”

Section: Strongly Interacting and Composite Dark Mattermentioning

confidence: 99%

Galactic Center gas clouds and novel bounds on ultralight dark photon, vector portal, strongly interacting, composite, and super-heavy dark matter

et al. 2019

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Cold gas clouds recently discovered hundreds of parsecs from the center of the Milky Way Galaxy have the potential to detect dark matter. With a detailed treatment of gas cloud microphysical interactions, we determine Galactic Center gas cloud temperatures, unbound electron abundances, atomic ionization fractions, heating rates, cooling rates, and find how these quantities vary with metallicity. Considering a number of different dark sector heating mechanisms, we set new bounds on ultra-light dark photon dark matter for masses 10 −22 − 10 −10 eV, vector portal dark matter coupled through a sub-MeV mass boson, and up to 10 60 GeV mass dark matter that interacts with baryons.

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Direct detection of bound states of asymmetric dark matter

Cited by 51 publications

References 103 publications

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

Terrestrial and martian heat flow limits on dark matter

Galactic Center gas clouds and novel bounds on ultralight dark photon, vector portal, strongly interacting, composite, and super-heavy dark matter

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