Coronal oscillations - Energy transport in the sun by magneto-atmospheric modes

Errors are demonstrated to exist in an eikonal approximation of the wave propagation in the solar atmosphere, and possible models for wave heating of the corona are considered. Consideration is given to data from the ATM instruments on board Skylab, from the OSO series satellites, and to studies of other stellar coronas with the IUE and Einstein Observatory. It is shown that Alfven waves propagating from the convection zone are not strong enough to heat the solar corona to the observed levels, which are actually hotter than those in the photosphere, although the corona has a less dense composition. A zone is argued to exist where magnetogravitosonic waves emerge in relatively stable condition, and have been detected in the solar wind. A linear analysis is presented to identify the region of origin of the upcoming waves, showing that slow vertical oscillations emerge above sunspots while slow magnetohydrodynamic waves do not.