  The ROSAT Galactic wind observations confirm that our Galaxy launches
supernova driven Galactic winds with wind speeds of about 150 km/s in the
Galactic plane. Galactic winds of this strength are incompatible with current
isotropic models for Cosmic Ray transport. In order to reproduce our local CRs
in the presence of Galactic winds, charged CRs are required to be much more
localized than in the standard isotropic GALPROP models. This requires that
anisotropic diffusion is the dominant diffusion mode in the interstellar
medium, particularly that the diffusion in the disk and in the halo are
different. In addition small scale phenomena such as trapping by molecular
cloud complexes and the structure of our local environment might influence the
secondary CR production rate and our local CR density gradients. We introduce
an anisotropic convection driven transport model (aCDM) which is consistent
with the Galactic wind observations by ROSAT. This also explains the large
bulge/disk ratio as observed by INTEGRAL. Furthermore such models predict an
increase in the $e^+/(e^++e^-)$-fraction as observed by PAMELA and HEAT, if the
synchrotron constraints in the 408 MHz and WMAP range are taken into account.
No additional contribution from Dark Matter is required. The aCDM is able to
explain the absence of a positron annihilation signal from molecular clouds as
observed by INTEGRAL by virtue of a mechanism which confines and isotropizes
CRs between MCs. We find that the EGRET excess of diffuse $\gamma$-rays
currently cannot be explained by astrophysical effects in this type of model
and that the interpretation of the EGRET excess as Dark Matter annihilation is
perfectly consistent with all observational constraints from local CR fluxes
and synchrotron radiation.
