  Weakly interacting massive particles (WIMPs) are a viable candidate for the
relic abundance of dark matter (DM) produced in the early universe. So far
WIMPs have eluded direct detection through interactions with baryonic matter.
Neutrino emission from accumulated WIMP annihilations in the solar core has
been proposed as a signature of DM, but has not yet been detected. These null
results may be due to small scale DM density fluctuations in the halo with the
density of our local region being lower than the average (around 0.3 GeV/cm^3
). However, the accumulated neutrino signal from WIMP annihilations in the
Galactic stellar disk would be insensitive to local density variations. Inside
the disk, dark matter can be captured by stars causing an enhanced annihilation
rate and therefore a potentially higher neutrino flux than what would be
observed from elsewhere in the halo. We estimate a neutrino flux from the WIMP
annihilations in the stellar disk to be enhanced by more than an order of
magnitude compared to the neutrino fluxes from the halo. We offer a
conservative estimate for this enhanced flux, based on the WIMP-nucleon
cross-sections obtained from direct-detection experiments by assuming a density
of around 0.3 GeV/cm^3 for the local DM. We also compare the detectability of
these fluxes with a signal of diffuse high energy neutrinos produced in the
Milky Way by the interaction of cosmic rays (CRs) with the interstellar medium
(ISM). These comparative signals should be observable by large neutrino
detectors.
