  Some differences between theoretical, numerical and observational
determinations of spectral slopes of solar wind turbulence are interpreted in
the thermodynamical sense. Confirmations of turbulent Kolmogorov slopes in
solar wind magnetic turbulence and magnetohydrodynamic simulations exhibit tiny
differences. These are used to infer about entropy generation in the turbulent
cascade and to infer about the anomalous turbulent collision frequency in the
dissipative range as well as the average energy input in solar wind turbulence.
Anomalous turbulent collision frequencies are obtained of the order of v < 200
Hz. The corresponding stationary solar wind magnetic energy input into magnetic
turbulence in the Kolmogorov inertial range is obtained to be of the order of
50 eV/s. Its thermal fate is discussed.
