Destruction of axion miniclusters in the Galaxy
  Previously, it has been established that axion dark matter (DM) is clustered
to form clumps (axion miniclusters) with masses $M\sim10^{-12}M_\odot$. The
passages of such clumps through the Earth are very rare events occurring once
in $10^5$ years. It has also been shown that the Earth's passage through DM
streams, which are the remnants of clumps destroyed by tidal gravitational
forces from Galactic stars, is a much more probable event occurring once in
several years. In this paper we have performed details calculations of the
destruction of miniclusters by taking into account their distribution in orbits
in the Galactic halo. We have investigated two DM halo models, the
Navarro-Frenk-White and isothermal density profiles. Apart from the Galactic
disk stars, we have also taken into account the halo and bulge stars. We show
that about 2-5% of the axion miniclusters are destroyed when passing near stars
and transform into axion streams, while the clump destruction efficiency
depends on the DM halo model. The expected detection rate of streams with an
overdensity exceeding an order of magnitude is 1-2 in 20 years. The possibility
of detecting streams by their tidal gravitational effect on gravitational-wave
interferometers is also considered.
