Excitation of oscillations in the magnetic network on the Sun

We examine the excitation of oscillations in the magnetic network of the Su n through the footpoint motion of photospheric magnetic flux tubes located in intergranular lanes. The motion is derived from a time series of high-re solution G-band and continuum filtergrams using an object-tracking techniqu e. We model the response of the flux tube to the footpoint motion in terms of the Klein-Gordon equation, which is solved analytically as an initial va lue problem for transverse (kink) waves. We compute the wave energy flux in upward-propagating transverse waves. In general we find that the injection of energy into the chromosphere occurs in short-duration pulses, which wou ld lead to a time variability in chromospheric emission that is incompatibl e with observations. Therefore, we consider the effects of turbulent convec tive flows on flux tubes in intergranular lanes. The turbulent flows are si mulated by adding high-frequency motions (periods 5-50 s) with an amplitude of 1 km s(-1). The latter are simulated by adding random velocity fluctuat ions to the observationally determined velocities. In this case, we find th at the energy flux is much less intermittent and can in principle carry ade quate energy for chromospheric heating.