It is often said that the blessing and curse of solar physics is that there is too much data. Although solar missions such as Yohkoh, SOHO and TRACE have shown the Sun's outer atmosphere with amazing clarity, they have also produced data of
higher complexity and information content than previous missions. While our view of the Sun has vastly improved, there has been less corresponding improvement in image analysis techniques. Typically, one observes the evolution of features in a sequence of byte-scaled intensity or intensity difference images. Such images allow qualitative assessments of features and structures, but they are limited for more quantitative or objective measurements.
Among the many advances in image processing techniques over the past decade, iscale/multiresolution methods are perhaps the most promising for quantitatively analyzing images. These methods have been used to model the human ability to view and comprehend phenomena on different spatial and temporal scales. These methods render the imaging processing by an observers' eyes and brains into a more objective framework. In this work, we present a preliminary
analysis of multiscale techniques as applied to solar image data. Specifically, we explore the use of the 2-d wavelet transform and related transforms with extreme ultraviolet and visible images of the solar corona.
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