A two-fluid slow solar wind model with proton temperature anisotropy and Alfven-wave turbulence

We present a one-dimensional slow solar-wind model that includes the magnetic field line curvature and low-frequency Alfven-wave (AW) turbulence. The dissipation mechanism for an anisotropic turbulent cascade used in this model is adopted on the basis of Chandran et al. 2011, which is restricted to the fast solar wind in a polar coronal hole. Here we extend this promising mechanism to slow wind model by considering the field line curvature. We also add terms in order to present the effect of the micro-instabilities on proton temperature isotropization. The numerical steady-state solutions are consistent with the observations, suggesting the idea that the fast and slow winds might share a common heating mechanism and the proton cyclotron instability might be an efficient process regulating the temperature anisotropy in the vicinity of 10-30 solar radii.