  The paper presents a new method for deriving turbulent heating of the solar
wind using plasma moments and magnetic field data. We develop the method and
then apply it to compute the turbulent heating of the solar wind proton plasma
at 1AU. The method employs two physical properties of the expanding solar wind
plasma, the wave-particle thermodynamic equilibrium, and the transport of
entropic rate. We analyze plasma moments and field datasets taken from Wind
S/C, in order to compute (i) the fluctuating magnetic energy, (ii) the
corresponding correlation length, and (iii) the turbulent heating rate. We
identify their relationships with the solar wind speed, as well as the
variation of these relationships relative to solar wind and interplanetary
coronal mass ejection plasma.
