Oscillating Composite Asymmetric Dark Matter. (arXiv:1907.11464v1 [hep-ph])

Oscillating Composite Asymmetric Dark Matter. (arXiv:1907.11464v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Ibe_M/0/1/0/all/0/1">Masahiro Ibe</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kobayashi_S/0/1/0/all/0/1">Shin Kobayashi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nagai_R/0/1/0/all/0/1">Ryo Nagai</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nakano_W/0/1/0/all/0/1">Wakutaka Nakano</a>

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
${cal O}(1),$GeV. In the ADM scenarios, composite dark matter is particularly
motivated, as it can naturally provide the DM mass in the ${cal O}(1),$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 gamma-ray from the
dwarf spheroidal galaxies.

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