Solar constraints on asymmetric dark matter
  The dark matter content of the Universe is likely to be a mixture of matter
and antimatter, perhaps comparable to the measured asymmetric mixture of
baryons and antibaryons. During the early stages of the Universe, the dark
matter particles are produced in a process similar to baryogenesis, and dark
matter freeze-out depends on the dark matter asymmetry and the annihilation
cross section (s-wave and p-wave annihilation channels). In these
\eta-parametrised asymmetric dark matter models (\eta-ADM), the dark matter
particles have an annihilation cross section close to the weak interaction
cross section, and a value of \eta-dark matter asymmetry close to the baryon
asymmetry \eta_B. Furthermore, we assume that dark matter scattering of
baryons, namely, the spin-independent scattering cross section, is of the same
order as the range of values suggested by several theoretical particle physics
models used to explain the current unexplained events reported in the
DAMA/LIBRA, CoGeNT and CRESST experiments. Here, we constrain \eta-ADM models
by investigating the impact of such a type of dark matter on the evolution of
the Sun, namely, the flux of solar neutrinos and helioseismology. We find that
dark matter particles with a mass smaller than 15 GeV, a spin-independent
scattering cross section on baryons of the order of a picobarn, and an
\eta-dark matter asymmetry with a value in the interval 10^{-12}-10^{-10},
would induce a change in solar neutrino fluxes in disagreement with current
neutrino flux measurements. A natural consequence of this model is suppressed
annihilation, thereby reducing the tension between indirect and direct dark
matter detection experiments, but the model also allows a greatly enhanced
annihilation cross section. All the cosmological \eta-asymmetric dark matter
scenarios that we discuss are in agreement with the current WMAP measured
values.
