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Indirect Detection of Self-Interacting Asymmetric Dark Matter
High Energy Physics - Phenomenology · Submitted 29 Mar 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We estimate the produced signal and explicitly demonstrate parameters for which the signal exceeds current observations.
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The abstract, sentence by sentence
Self-interacting dark matter resolves the issue of cuspy profiles that appear in non-interacting cold dark matter simluations; it may additionally resolve the so-called "too big to fail" problem in structure formation. Asymmetric dark matter provides a natural explanation of the comparable densities of baryonic matter and dark matter. In this paper, we discuss unique indirect detection signals produced by a minimal model of self-interacting asymmetric scalar dark matter. Through the formation of dark matter bound states, a dark force mediator particle may be emitted; the decay of this particle may produce an observable signal. We estimate the produced signal and explicitly demonstrate parameters for which the signal exceeds current observations.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Self-interacting dark matter resolves the issue of cuspy profiles that appear in non-interacting cold dark matter simluations; it may additionally resolve the so-called "too big to fail" problem in structure formation. | background 1.00 | 0.05 | 0.04 | asserted 0.52 |
| s1 | Asymmetric dark matter provides a natural explanation of the comparable densities of baryonic matter and dark matter. | background 1.00 | 0.04 | 0.03 | asserted 0.76 |
| s2 | In this paper, we discuss unique indirect detection signals produced by a minimal model of self-interacting asymmetric scalar dark matter. | contribution 1.00 | 0.82 | 0.14 | asserted 0.92 |
| s3 | Through the formation of dark matter bound states, a dark force mediator particle may be emitted; the decay of this particle may produce an observable signal. | method 0.62 | 0.13 | 0.11 | hedged possibility 1.00 |
| s4 | We estimate the produced signal and explicitly demonstrate parameters for which the signal exceeds current observations. | result 0.85 | 0.95 | 0.58 | asserted 1.00 |
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The paper
Original abstract
Self-interacting dark matter resolves the issue of cuspy profiles that appear in non-interacting cold dark matter simluations; it may additionally resolve the so-called "too big to fail" problem in structure formation. Asymmetric dark matter provides a natural explanation of the comparable densities of baryonic matter and dark matter. In this paper, we discuss unique indirect detection signals produced by a minimal model of self-interacting asymmetric scalar dark matter. Through the formation of dark matter bound states, a dark force mediator particle may be emitted; the decay of this particle may produce an observable signal. We estimate the produced signal and explicitly demonstrate parameters for which the signal exceeds current observations.
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References
How the literature uses it
26 arXiv papers cite this in 38 sentences
Papers citing it · 27 sentences without a confident label
Uses its method or tool 4 papers
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[ref] , we compute the overlap integrals [ref] using the identity [ref]
Radiative bound-state formation in unbroken perturbative non-Abelian theories and implications for dark matter · Overlap integrals for capture into the ground state · 0.97
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Using the identity [ref] , [equation] we find the squared form factor after averaging over the angle between $p$ and $k$ to be [equation] where $ξ=1/(a_0 p)$ and $η=1/a_0$.
Stable Bound States of Asymmetric Dark Matter · Two-body Bound States · 0.94
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[ref] , we derive the Coulomb limit of the overlap integrals using the identity [ref]
Higgs-mediated bound states in dark-matter models · Overlap integrals · 0.89
Compares with it 1 paper
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The field-theoretic formalism developed in this work has several advantages in comparison to previous quantum mechanical calculations [ref] .
Dark-matter bound states from Feynman diagrams · Introduction · 0.91
Cites it as support 1 paper
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In fact, in a variety of models, bound-state formation (BSF) can be faster than annihilation [ref] .
Bound states of WIMP dark matter in Higgs-portal models. Part II. Thermal decoupling · Introduction · 0.96
Cites it as background 5 papers
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[ref] , the issue has been investigated more systematically in a series of recent studies [ref] .
Dark Matter's secret liaisons: phenomenology of a dark U(1) sector with bound states · Introduction · 0.86
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Indirect signals of BSF in the center of the Milky Way has been studied for DM with no particle-antiparticle asymmetry, as well as for asymmetric DM [ref] .
Dark matter bound-state formation in the Sun · Introduction · 0.92
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This type of analysis has been used largely for asymmetric dark matter [ref] , considered the prototypical example of non-annihilating dark matter.
Bounds on self-interacting fermion dark matter from observations of old neutron stars · Introduction · 0.98
What it cites · 63 sentences without a confident label
Builds on 1 paper
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We extended the analysis of Ref. [ref] to $m_S = 10 TeV$ in Appendix [ref]; this showed that for $m_σ= .5 MeV$ and $m_S = 10 TeV$, we prefer to take $α= A_σS^2 16 πm_S^2 ≲.93$ although this may be loosened somewhat.
Halo Shape and Relic Density Exclusions of Sommerfeld-Enhanced Dark Matter Explanations of Cosmic Ray Excesses · Choice of parameters · 0.97
Uses data or values from 7 papers
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To be consistent with astrophysical data, we then must have $σ_T^max m_S ≤100 GeV^-3$ [ref] ; the above numbers correspond to $.2 GeV^-3$ and $9 GeV^-3$.
Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential · Choice of parameters · 0.89
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If $v_max ∼10 km s$, then the astrophysical constraints are consistent if $22.7 m_σ^2 m_S ≲35 cm^2 g = 16000 GeV^-3$ [ref] ; we will verify that we satisfy this condition below.
Subhaloes in Self-Interacting Galactic Dark Matter Haloes · Choice of parameters · 0.84
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The analytic fit for $σ_T$, the distribution functions, and the relevant parameters for NGC 720 are all available in [ref] .
Halo Shape and Relic Density Exclusions of Sommerfeld-Enhanced Dark Matter Explanations of Cosmic Ray Excesses · Extension of Bounds From Halo Ellipticity · 0.93
Cites as support 4 papers
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We have noted above that the calculated cross section does not include a Sommerfeld enhancement, because some analysis suggest that such large factors are unreliable [ref] .
Limits on Threshold and "Sommerfeld" Enhancements in Dark Matter Annihilation · Decay of the $σ$ Bosons and Resulting Signal · 0.97
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We note that simulations support the assumption of a locally Gaussian velocity distribution even for cold dark matter [ref] , and the isothermal approximation is better for self-interacting dark matter [ref] , [ref] .
Phase-space structure in the local dark matter distribution and its signature in direct detection experiments · Dark Matter in the Milky Way · 0.99
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We note that simulations support the assumption of a locally Gaussian velocity distribution even for cold dark matter [ref] , and the isothermal approximation is better for self-interacting dark matter [ref] , [ref] .
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure · Dark Matter in the Milky Way · 0.99
Cites as background 23 papers
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It has previously been observed that many models of self-interacting dark matter, including supersymmetric models, permit the existence of dark matter bound states [ref] .
WIMPonium · Dark Matter Bound States · 0.97
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(For a recent review, see, e.g., Ref. [ref] .) Such asymmetric dark matter does not annihilate at present, and, as long as it is stable, no indirect detection signals are expected in gamma rays or neutrinos.
Review of asymmetric dark matter · Introduction · 0.95
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First, we assume that the correct abundance of $S$ particles is determined by some process that is similar to baryogenesis or related to baryogenesis, as in models reviewed in Ref. [ref] .
Hylogenesis: A Unified Origin for Baryonic Visible Matter and Antibaryonic Dark Matter · Dark Matter in the Milky Way · 0.90
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