  If dark matter particle can be decelerated due to its dissipative self
scattering, except for sinking at the galaxy scale to speed up structure
formation, it can also be accreted onto local celestial bodies such as the Sun,
forming a compact halo. With some simplified assumptions we develop the
Boltzmann equation set based on the partition function of the elliptical
orbits, and numerically solve it for the accretion process. We find that the
orbited dark matter particles will form a halo around the Sun, with the density
profile well fitted to be proportional to $r^{-1.6}$ in a wide range of radius.
While around the earth such local halo contribution is always several orders
below the galactic component, in a very small region centered around the Sun
the sunk dark matter particles can lead to a halo density several orders larger
than the background galactic component, in particular in the parameter region
of small deceleration speed and large cross section, which is still consistent
with current constraints. Such potential dark matter local halo with
significantly enhanced density will be a very interesting source for dark
matter indirect detection if the corresponding channel exists, we discuss the
possibility of the gamma-ray spectrum in the solar direction in some detail as
an example.
