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Alfv\'{e}nic component of MHD turbulence damps Alfv\'{e}nic waves. Theconsequences of this effect are important for many processes, from cosmic ray(CR) propagation to launching outflows and winds in galaxies and othermagnetized systems. We discuss the differences in the damping of the streaminginstability by turbulence and the damping of a plane parallel wave. The formertakes place in the system of reference aligned with the local direction ofmagnetic field along which CRs stream. The latter is in the reference frame ofthe mean magnetic field and traditionally considered in plasma studies. We alsocompare the turbulent damping of streaming instability with ion-neutralcollisional damping, which becomes the dominant damping effect at asufficiently low ionization fraction. Numerical testing and astrophysicalimplications are also discussed.

Damping of Alfv\'{e}n waves in MHD turbulence and implications for cosmic ray streaming instability and galactic winds