  In hydrodynamic turbulence, it is well established that the length of the
dissipation scale depends on the energy cascade rate, i.e., the larger the
energy input rate per unit mass, the more the turbulent fluctuations need to be
driven to increasingly smaller scales to dissipate the larger energy flux.
Observations of magnetic spectral energy densities indicate that this intuitive
picture is not valid in solar wind turbulence. Dissipation seems to set in at
the same length scale for different solar wind conditions independently of the
energy flux. To investigate this difference in more detail, we present an
analytic dissipation model for solar wind turbulence at electron scales, which
we compare with observed spectral densities. Our model combines the energy
transport from large to small scales and collisionless damping, which removes
energy from the magnetic fluctuations in the kinetic regime. We assume
wave-particle interactions of kinetic Alfv\'{e}n waves (KAW) to be the main
damping process. Wave frequencies and damping rates of KAW are obtained from
the hot plasma dispersion relation. Our model assumes a critically balanced
turbulence, where larger energy cascade rates excite larger parallel
wavenumbers for a certain perpendicular wavenumber. If the dissipation is
additionally wave driven such that the dissipation rate is proportional to the
parallel wavenumber - as with KAW - then an increase of the energy cascade rate
is counter-balanced by an increased dissipation rate for the same perpendicular
wavenumber leading to a dissipation length independent of the energy cascade
rate.
