Abstract

The asymmetric dark matter (ADM) scenario can solve the coincidence problem between the baryon and the dark matter (DM) abundance when the DM mass is of mathcal{O} (1) GeV. In the ADM scenarios, composite dark matter is particularly motivated, as it can naturally provide the DM mass in the mathcal{O} (1) GeV range and a large annihilation cross section simultaneously. In this paper, we discuss the indirect detection constraints on the composite ADM model. The portal operators connecting the B − L asymmetries in the dark and the Standard Model(SM) sectors are assumed to be generated in association with the seesaw mechanism. In this model, composite dark matter inevitably obtains a tiny Majorana mass which induces a pair-annihilation of ADM at late times. We show that the model can be efficiently tested by the searches for the γ-ray from the dwarf spheroidal galaxies and the interstellar electron/positron flux.

Highlights

  • In this paper, we discuss the indirect detection of the composite asymmetric dark matter (ADM) model in [24,25,26]

  • The composite ADM model is motivated as it provides the DM mass of O(1) GeV and a large annihilation cross section simultaneously

  • We discussed the indirect detection of the composite ADM where the portal operators of the B − L asymmetry is generated in association with the seesaw mechanism

Read more

Summary

A model of composite ADM

We briefly review the composite ADM model in [24,25,26]. The model is based on Ng-generation dark quarks with SU(3)D × U(1)D gauge symmetry. The dark quarks are the fundamental representations of SU(3)D They are charged under the dark QED and the B − L in analogy to the up-type and the down-type quarks in the visible sector (see table 1). They have tiny masses, Lmass = mU U U + mDD D + h.c. When the B − L asymmetry is thermally distributed between the visible and the dark sectors, the ratio of the B − L asymmetry stored in each sector is given by ADM/ASM = 44Ng/237 for the B − L charges given in table 1 [44].2. The dark photon obtains its mass by the dark Higgs mechanism, and it decays into the visible fermions thought the kinetic mixing with the visible QED photon, Lγ

Fμν F μν
The Majorana mass of the dark neutron
Washout interactions and on-shell portal
Gamma-ray flux from the dwarf spheroidal galaxies
Constraints on parameter space
Conclusions
A Final state radiation in the dark photon decay
Result
Findings
B Sommerfeld enhancement
Full Text
Published version (Free)

Talk to us

Join us for a 30 min session where you can share your feedback and ask us any queries you have

Schedule a call