Signatures of dark matter burning in nuclear star clusters
  In order to characterize how dark matter (DM) annihilation inside stars
changes the aspect of a stellar cluster we computed the evolution until the
ignition of the He burning of stars from 0.7 to 3.5 M_sun within halos of DM
with different characteristics. We found that, when a cluster is surrounded by
a dense DM halo, the positions of the cluster' stars in the H-R diagram have a
brighter and hotter turn-off point than in the classical scenario without DM,
therefore giving the cluster a younger appearance. The high DM densities
required to produce these effects are expected only in very specific locations,
such as near the center of our Galaxy. In particular, if DM is formed by the 8
GeV WIMPs recently invoked to reconcile the results from direct detection
experiments, then this signature is predicted for halos of DM with a density
rho_DM = 3 \cdot 10^5 GeV cm^3. A DM density gradient inside the stellar
cluster would result in a broader main sequence, turn-off and red giant branch
regions. Moreover, we found that for very high DM halo densities the bottom of
the isochrones in the H-R diagram rises to higher luminosities, leading to a
characteristic signature on the stellar cluster. We argue that this signature
could be used to indirectly probe the presence of DM particles in the location
of a cluster.
