Turbulent power and dissipation in the solar transition zone

The power spectrum of the spatial velocity fluctuations of the solar transition zone are determined from high-resolution telescope and spectrograph solar spectra of C IV. It is found that virtually all of the power resides at higher wavenumbers and that the spectrum is flatter than predicted for the inertial range of a turbulent fluid. The results suggest that the small-scale fluctuations are maintained by a driving mechanism such as magnetic reconnection or wave motions produced in the photosphere.