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Some 8000 images obtained with the SECIS fast-frame CCD camera instrumentlocated at Lusaka, Zambia, during the total eclipse of 21 June 2001 have beenanalyzed to search for short-period oscillations in intensity that could be asignature of solar coronal heating mechanisms by MHD wave dissipation. Imageswere taken in white- light and Fe XIV green-line (5303 A) channels over 205seconds (frame rate 39 s-1), approximately the length of eclipse totality atthis location, with a pixel size of four arcseconds square. The data are ofconsiderably better quality than were obtained during the 11 August 1999 totaleclipse, observed by us (Rudawy et al.: Astron. Astrophys. 416, 1179, 2004), inthat the images are much better exposed and enhancements in the drive system ofthe heliostat used gave a much improved image stability. Classical Fourier andwavelet techniques have been used to analyze the emission at 29518 locations,of which 10714 had emission at reasonably high levels, searching for periodicfluctuations with periods in the range 0.1-17 seconds (frequencies 0.06-10 Hz).While a number of possible periodicities were apparent in the wavelet analysis,none of the spatially and time-limited periodicities in the local brightnesscurves was found to be physically important. This implies that the pervasiveAlfven wave-like phenomena (Tomczyk et al.: Science 317, 1192, 2007) usingpolarimetric observations with the CoMP instrument do not give rise tosignificant oscillatory intensity fluctuations.

Search for Rapid Changes in the Visible-Light Corona during the 21 June 2001 Total Solar Eclipse