  The question how the outer solar atmosphere is heated from solar photospheric
temperatures of about 5800K up to solar chromospheric and coronal temperatures
of about 20.000K and millions of degrees respectively, remained without any
satisfying answer for centuries. On 4 May 2005, I recorded several time series
of Halpha line scans with the GREGOR Fabry-Perot Interferometer, still deployed
at the German Vacuum Tower Telescope (VTT), for different solar limb and
on-disk positions as well as for quiet sun at solar disk center. The spatially
and temporally highly resolved time series of Halpha line parameters reveal the
entire and detailed complexity as well as the overwhelming dynamics of spicules
covering the entire solar disk, thus apparently confirming spicules as the
potential driver of chromospheric heating for both the Sun and sun-like stars,
with an expected mass flux larger than 100 times that of the solar wind.
Spicules seem to be the result of the interaction of the highly dynamic
photospheric quiet-sun or active-region small-scale magnetic field, which is
dominated by convective processes and is predominantly located in intergranular
lanes and at meso- or supergranular scales.
