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Total Solar Eclipse 2006

Results

Solar Eclipse 2006 Programs

Step to Step by HRC Team in Eclipse

Results of International Friends

This images have been selected among more than 200 photos and digital images, during total solar eclipse 2006. The movie has been made by 30 images. These images have been taken by: Ehsan Eslahi, Dr Mohammad Rafienia and Mohammad Akoochekian via Canon and Sony digital cameras. The movie is available in 2 versions: Real Media to watch it as live and QuickTime Movie for download.

Polarization Changes in Corona

We used a linear polarization filter to study corona magnetic fields. The filter angle changed from 0 to 170 (deg.) and camera recorded a photo in each angle. Then the images were analyzed by Sun Processor to obtain different results, but the most important result was drawing corona magnetic field lines (their images over sky sheet). Now the first results are available. Final result will be published after complete investigation and studying.

	Investigatin of Magnetic field intensity at different filter angles, 1st type (QuickTime Movie: 2.9 MB ) This Movie shows change of polarization intensity of each coronal point at different polarization angle. Analyzed by SUN PROCESSOR
	Investigatin of Magnetic field intensity at different filter angles, 2nd type (QuickTime Movie: 2.9 MB ) This Movie shows change of polarization intensity of each coronal point at different polarization angle and compares them with real image of corona. Analyzed by SUN PROCESSOR
	Changes of Corona Shape with Polaroid Angle (QuickTime Movie: 2.5 MB) This Movie shows change of corona shape at different polarization angle.
	(3D) Changes of Corona Shape with Polaroid Angle (QuickTime Movie: 1.1 MB) This Movie shows change of corona shape in 3D mode at different polarization angle. The higher points have more intensive brightness than others. Analyzed by SUN PROCESSOR

Then Sun Processor analyzed all of polarized images by a mathematical algorithm. Its final results is shown in following images. But this is the first step, because it must be compared with other standard models and developed to the best scientific level. Lines direction and length at each point help us to estimate direction and intensity of magnetic field line of that point. You can see that the field strength near solar surface is nearly zero, but the increase very fast at height of 0.6 to 0.8 of solar radii.

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