  We develop a 1D solar-wind model that includes separate energy equations for
the electrons and protons, proton temperature anisotropy, collisional and
collisionless heat flux, and an analytical treatment of low-frequency,
reflection-driven, Alfven-wave turbulence. To partition the turbulent heating
between electron heating, parallel proton heating, and perpendicular proton
heating, we employ results from the theories of linear wave damping and
nonlinear stochastic heating. We account for mirror and oblique firehose
instabilities by increasing the proton pitch-angle scattering rate when the
proton temperature anisotropy exceeds the threshold for either instability. We
numerically integrate the equations of the model forward in time until a steady
state is reached, focusing on two fast-solar-wind-like solutions. These
solutions are consistent with a number of observations, supporting the idea
that Alfven-wave turbulence plays an important role in the origin of the solar
wind.
