  Solar wind turbulence is dominated by Alfv\'{e}nic fluctuations but the power
spectral exponents somewhat surprisingly evolve toward the Kolmogorov value of
-5/3, that of hydrodynamic turbulence. We show that at 1AU the turbulence
decomposes linearly into two coexistent components perpendicular and parallel
to the local average magnetic field. The first of these is consistent with
propagating Alfv\'{e}n wavepackets and shows the scaling expected of
Alfv\'{e}nic turbulence, namely Irosnikov- Kraichnan. The second shows
Kolmogorov scaling which we also find in the number and magnetic energy
density, and Poynting flux.
