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Large-scale galactic winds driven by stellar feedback are one phenomenon thatinfluences the dynamical and chemical evolution of a galaxy, redistributingmaterial throughout the circumgalatic medium. Non-thermal feedback fromgalactic cosmic rays (CRs) -high-energy charged particles accelerated insupernovae and young stars - can impact the efficiency of wind driving. Thestreaming instability limits the speed at which they can escape. However, inthe presence of turbulence, the streaming instability is subject to suppressionthat depends on the magnetization of turbulence given by its Alfv\'en Machnumber. While previous simulations that relied on a simplified model of CRtransport have shown that super-Alfv\'enic streaming of CRs enhances galacticwinds, in the present paper we take into account a realistic model of streamingsuppression. We perform three-dimensional magnetohydrodynamic simulations of asection of a galactic disk and find that turbulent damping dependent on localmagnetization of turbulent interstellar medium (ISM) leads to more spatiallyextended gas and CR distributions compared to the earlier streamingcalculations, and that scale-heights of these distributions increase forstronger turbulence. Our results indicate that the star formation rateincreases with the level of turbulence in the ISM. We also find that theinstantaneous wind mass loading is sensitive to local streaming physics withthe mass loading dropping significantly as the strength of turbulenceincreases.

Role of Cosmic Ray Streaming and Turbulent Damping in Driving Galactic Winds