Outer corona enhanced structure

This image is specially processed using the Corona 3.0 software to enhance the faint structures in the solar corona.
During the 2005 total solar eclipse the solar activity cycle was about two years before the minimum and the coronal shape had a lot of features typical for the minimum. Especially both magnetic poles of the Sun are well recognizable by typical simple structure of powerlines which are well visualized by inhomogeneity of plasma in the solar corona.

Date08. 04. 2005
Time2nd contact 21:15:05 UT, 3rd contact 21:15:37 UT
Total eclipse duration 32 s
PlacePacific ocean aboard the MV Galapagos Legend (about 2100 km west from the Galapagos)
Coordinate1° 19.554' S, 109° 30.190' W
ConditionsClear sky, altitude of the Sun above the horizon 60°
OpticsCanon 500 mm f/4 IS lens
CameraCanon EOS 1Ds Mark II digital camera
Exposure1/2000 s - 1/15 s
ProcessingComposition of 8 images. Images were aligned by means of phase correlation, calibrated and composed using a new, for this purpose newly developed, software LDIC 1.0, processed using Corona 3.0 in order to visualize coronal structures. Final processing was done using ACC 6.0 software.
Image processing by Miloslav Druckmüller
SoftwarePhaseCorr 3.0, LDIC 1.0, Corona 3.0, Sofo ACC 6.0
NoteThe graph above the table shows the average values of the relative number of sunspots in which the red arrow indicates the time of 2005 eclipse. Graph was created according to data from Sunspot Index Data Center, Brussels.
OrientationThe image has the standard orientation i.e. North top, East left
More infoOriginal set of images
Copyright© 2005 Miloslav Druckmüller, Fred Espenak

Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
Page last update: 27.11.2019