Cosmic rays passing through large astrospheres can be efficiently cooled
inside these "cavities" in the interstellar medium. Moreover, the energy
spectra of these energetic particles are already modulated in front of the
astrospherical bow shocks. We study the cosmic ray flux in and around lambda
Cephei as an example for an astrosphere. The large-scale plasma flow is modeled
hydrodynamically with radiative cooling. We studied the cosmic ray flux in a
stellar wind cavity using a transport model based on stochastic differential
equations. The required parameters, most importantly, the elements of the
diffusion tensor, are based on the heliospheric parameters. The magnetic field
required for the diffusion coefficients is calculated kinematically. We discuss
the transport in an astrospheric scenario with varying parameters for the
transport coefficients. We show that large stellar wind cavities can act as
sinks for the galactic cosmic ray flux and thus can give rise to small-scale
anisotropies in the direction to the observer. Small-scale cosmic ray
anisotropies can naturally be explained by the modulation of cosmic ray spectra
in huge stellar wind cavities
