Supersymmetric Resonant Dark Matter: a Thermal Model for the AMS-02 Positron Excess

Abstract

We construct a thermal dark matter model with annihilation mediated by a resonance to explain the positron excess observed by PAMELA, Fermi-LAT and AMS-02, while satisfying constraints from cosmic microwave background (CMB) measurements. The challenging requirement is that the resonance has twice the dark matter mass to one part in a million. We achieve this by introducing an $SU(3{)}_f$ dark flavor symmetry that is spontaneously broken to $SU(2{)}_f\times U(1{)}_f$. The resonance is the heaviest state in the dark matter flavor multiplet and the required mass relation is protected by the vacuum structure and supersymmetry from radiative corrections. The pseudo-Nambu Goldstone Bosons (PNGB's) from the dark flavor symmetry breaking can be slightly lighter than one GeV and dominantly decay into two muons just from kinematics, with subsequent decay into positrons. The PNGB's are produced in resonant dark matter semi-annihilation, where two dark matter particles annihilate into an anti-dark matter particle and a PNGB. The dark matter mass in our model is constrained to be below around 1.9 TeV from fitting thermal relic abundance, AMS-02 data and CMB constraints. The superpartners of Standard Model (SM) particles can cascade decay into a light PNGB along with SM particles, yielding a correlated signal of this model at colliders. One of the interesting signatures is a resonance of a SM Higgs boson plus two collimated muons, which has superb discovery potential at LHC Run 2.

34 pages, 11 figures

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• Heavy dark matter particle annihilation in dwarf spheroidal galaxies: radio signals at the SKA telescope
• The DAMPE excess and gamma-ray constraints
• Leptophilic-portal Dark Matter in the Light of AMS-02 positron excess
• Indirect effects of dark matter
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• Gauge-Independent Approach to Resonant Dark Matter Annihilation
• Consistent explanation for the cosmic-ray positron excess in $p$-wave Breit-Wigner enhanced dark matter annihilation
• Reexamine the dark matter scenario accounting for the positron excess in a new cosmic ray propagation model
• Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios
• Multicomponent Dark Matter in the Light of CALET and DAMPE