A study of a quiet solar network region structure and dynamics using ground and space based observations

We present a detailed study of a very quiet solar region, using data from an observational campaign that involved ground based and space born instruments. The region was observed by the Dutch Open Telescope, the XRT, SOT and EIS instruments onboard Hinode, TRACE and the MDI onboard SoHO. This combination of instruments offers a complete tomographic view of the atmospheric layers from the photosphere to the corona and allows a) the determination of its magnetic and temperature structure b) the correspondence between fine structure and jet-like events at different atmospheric heights c) the study of wave propagation through the atmospheric layers. A calculation of the current-free magnetic field vector up to the corona shows that the network structure persists up to coronal temperatures and consists of a multitude of flux tubes that connect to different network and internetwork areas and reach different heights and temperatures. At least some of the jet like structure s observed in the Hα line, around the network, have a counterpart in the overlying atmosphere. We study their evolution in the different atmospheric heights/temperatures. We also determine the height of the magnetic canopy, the interface between the completely magnetized plasma of the chromosphere/transition region and the underlying photosphere. The distribution of the power of the acoustic oscillations and its dependence on the inclination of the magnetic field shows that, at the height of the magnetic canopy, acoustic waves undergo conversion and transmission. This finding is also supported by the measured phase differences between oscillations at different heights. Fast waves reflect at the turning height and form standing waves while slow waves propagate along the slanted magnetic field lines of the network.