An observational study of the dynamic behavior of flux tubes.

摘要

The solar chromosphere and corona have radiative losses which require a huge input of energy from the solar surface. Exactly how this energy is transported to the higher layers is not well understood. Evidence is mounting that chromospheric and coronal heating are tied intimately to magnetic fields on the solar surface, either through wave motions generated by the turbulence of solar granulation or stresses caused by the slow movement of magnetic fields as they are pushed by flows on the solar surface.; This study investigated, observationally, the role of magnetohydrodynamic waves in heating the chromosphere and corona. Because magnetic structures occur on small spatial scales at the solar surface, a parallel study of curvature sensing techniques for solar adaptive optics was also carried out.; The curvature sensing technique developed herein works well in measuring static aberrations in solar telescopes. Its more exciting application is in real-time adaptive optics, a possibility still under investigation.; The observational study of magnetic flux tube dynamics found oscillations in both the Doppler velocity and longitudinal magnetic field at wave periods of five minutes, corresponding to the frequency band of the solar p-mode oscillations. Acoustic and magnetic power maps show the power to be very localized. The acoustic power is greatest in regions of the penumbra, while magnetic power is located at the umbral/penumbral boundary. Magnetic and velocity oscillations had a phase difference which varied according to frequency.