How compact stars challenge our view about dark matter
  It is by now well established that non-relativistic matter in the Universe is
dominated by dark matter, the origin and nature of which still remains a
mystery. Although the collisionless dark matter paradigm works very well at
large distances, a few puzzles at galactic scales arise. These problems may be
tackled assuming a self-interacting dark matter. If dark matter is accumulated
inside a star it will modify its evolution and its properties, such as
mass-to-radius profiles and frequency oscillation modes. Asteroseismology is a
relatively new, powerful tool that allows us to constrain dark matter models,
offering us complementary bounds to the results coming from other means, such
as collider or direct searches. I will present here the main results we have
obtained assuming that the dark matter particle is a boson, which inside a star
is modelled as a Bose-Einstein condensate with a polytropic equation-of-state.
We have computed i) the radial and non-radial oscillation modes of light clumps
of dark matter made of ultra light repulsive scalar fields, and ii) the
mass-to-radius profiles as well the frequencies of radial modes of admixed dark
matter strange quark stars.
