A search at two eclipses for short-period waves that heat the corona

As part of a study of the cause of solar coronal heating, we searched for h igh-frequency (similar to1 Hz) intensity oscillations in coronal loops in t he [Fe XIV] coronal green line. We summarize results from observations made at the 3 November 1994, total solar eclipse from the International Astrono mical Union site in Putre, Chile, through partly cloudy skies, and at the 2 6 February 1998 total solar eclipse from Nord, Aruba, through clear skies. We discuss the image reduction and analysis of two simultaneous series of c oronal CCD images digitized at 10 Hz for a total time of 160 s in Chile. On e series of images was taken through a filter isolating the 5303 Angstrom [ Fe XIV] coronal green line and the other through a 100 Angstrom filter in t he nearby K-corona continuum. We then discuss the modifications made for th e 1998 eclipse, and the image reduction and analysis for those image sequen ces. After standard calibrations and image alignment of both data sets, we use Fourier analysis to search in the [Fe XIV] channel for intensity oscill ations in loops at the base of the corona. Such oscillations in the 1-Hz ra nge are predicted as a result of density fluctuations from the resonant abs orption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could p rovide sufficient energy to heat the corona. At neither eclipse do we find evidence for oscillations in the [Fe XIV] green line at a level greater tha n 2% of coronal intensity.