  We develop a formalism that treats the calculation of solar kinetic energy
and cross helicity spectra in an equal manner to that of magnetic energy and
helicity spectra. The magnetic helicity spectrum is shown to be equal to the
vertical part of the current helicity spectrum divided by the square of the
wavenumber. For the cross helicity, we apply the recently developed two-scale
approach globally over an entire active region to account for the sign change
between the two polarities. Using vector magnetograms and Dopplergrams of NOAA
11158 and 12266, we show that kinetic and magnetic energy spectra have similar
slopes at intermediate wavenumbers, where the contribution from the granulation
velocity has been removed. At wavenumbers around 0.3 Mm$^{-1}$, the magnetic
helicity is found to be close to its maximal value. The cross helicity spectra
are found to be within about 10% of the maximum possible value. Using the
two-scale method for NOAA 12266, the global cross helicity spectrum is found to
be particularly steep, similarly to what has previously been found in
theoretical models of spot generation. In the quiet Sun, by comparison, the
cross helicity spectrum is found to be small.
