Quasi-degenerate dark matter for DAMPE excess and 3.5 keV line

Gu, Ping

doi:10.1007/s11433-018-9255-x

Cited by 7 publications

(1 citation statement)

References 51 publications

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“…Recently, the DAMPE collaboration reported its first result of the total CR e ± spectrum in the energy range from 25 GeV to 4.6 TeV [17]. Many studies have been performed to explain the tentative features in this spectrum [18,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,36,37,38,39,40,41,42,43,44,45].…”

Section: Introductionmentioning

confidence: 99%

Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

Wang

Lin

et al. 2018

Sci. China Phys. Mech. Astron.

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Many studies have shown that either the nearby astrophysical source or dark matter (DM) annihilation/decay is required to explain the origin of high energy cosmic ray (CR) e ± , which are measured by many experiments, such as PAMELA and AMS-02. Recently, the Dark Matter Particle Explorer (DAMPE) collaboration has reported its first result of the total CR e ± spectrum from 25 GeV to 4.6 TeV with high precision. In this work, we study the DM annihilation and pulsar interpretations of the DAMPE high energy e ± spectrum. In the DM scenario, the leptonic annihilation channels to τ + τ − , 4µ, 4τ , and mixed charged lepton final states can well fit the DAMPE result, while the µ + µ − channel has been excluded. In addition, we find that the mixed charged leptons channel would lead to a sharp drop at ∼ TeV. However, these DM explanations are almost excluded by the observations of gamma-ray and CMB, unless some complicated DM models are introduced. In the pulsar scenario, we analyze 21 nearby known pulsars and assume that one of them is the primary source of high energy CR e ± . Considering the constraint from the Fermi-LAT observation of the e ± anisotropy, we find that two pulsars are possible to explain the DAMPE data. Our results show that it is difficult to distinguish between the DM annihilation and single pulsar explanations of high energy e ± with the current DAMPE result.

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Section: Introductionmentioning

confidence: 99%

Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

Wang

Lin

et al. 2018

Sci. China Phys. Mech. Astron.

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Two-mediator dark matter models and cosmic electron excess

Liu

2019

J. High Energ. Phys.

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The cosmic electron energy spectrum recently observed by the DAMPE experiment exhibits two interesting features, including a break around 0.9 TeV and a sharp resonance near 1.4 TeV. In this analysis, we propose a dark matter explanation to both exotic features seen by DAMPE. In our model, dark matter annihilates in the galaxy via two different channels that lead to both a narrow resonance spectrum near 1.4 TeV and electron excess events over an extended energy range thus generating the break structure around TeV. The two annihilation channels are mediated by two gauge bosons that interact both with dark matter and with the standard model fermions. Dark matter annihilations through the s-channel process mediated by the heavier boson produce monoenergetic electron-positron pairs leading to the resonance excess. The lighter boson has a mass smaller than the dark matter such that they can be on-shell produced in dark matter annihilations in the galaxy; the lighter bosons in the final state subsequently decay to generate the extended excess events due to the smeared electron energy spectrum in this process. We further analyze constraints from various experiments, including HESS, Fermi, AMS, and LHC, to the parameter space of the model where both excess events can be accounted for. In order to interpret the two new features in the DAMPE data, dark matter annihilation cross sections in the current galaxy are typically much larger than the canonical thermal cross section needed for the correct dark matter relic abundance. This discrepancy, however, is remedied by the nonperturbative Sommerfeld enhancement because of the existence of a lighter mediator in the model.where we use R = 3.5 kpc, α = 2, β = 2 and γ = 0 [63]. The value of ρ s in all the above profiles are chosen such that the local DM density is normalized to ρ χ (8.5 kpc) = 0.39 GeV/cm 3 . We compute the HESS J-factors for these DM profiles using Eq. (6.2) J NFW = 2.25 × 10 21 GeV 2 /cm 5 , J E = 4.41 × 10 21 GeV 2 /cm 5 , J iso = 7.23 × 10 19 GeV 2 /cm 5 .(A.4)HESS collaboration [54] provides the J-factors for two profiles: J NFW = 2.67×10 21 GeV 2 /cm 5 and J E = 4.92 × 10 21 GeV 2 /cm 5 . Thus our calculation here yields slightly smaller J-factors than HESS. We use the J NFW and J E values provided by HESS [54] in the rescaling method to be described in Appendix (B). Because the J-factor for the isothermal profile is not given explicitly by HESS [54], we use our calculated J iso value in the analysis.

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Editorial

Cai

Zhou

2018

Sci. China Phys. Mech. Astron.

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Quasi-degenerate dark matter for DAMPE excess and 3.5 keV line

Cited by 7 publications

References 51 publications

Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

Two-mediator dark matter models and cosmic electron excess

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