Image

Solar corona through clouds

This image has no precedent in MMV-project archive. I have never processed total solar eclipse images significantly influenced by clouds. There were two reasons for that. The first one was that I was convinced that it makes no sense because no fine coronal structures would be visible. The second one was misgiving that I am able to create a software which would align and compose correctly images with different exposures containing moving clouds. Finally I tried to process the images even though the solar corona was partially obscured by clouds because no other images were available from Kenya and I knew that the relatively clear part of the image contains very interesting CME which is only partially visible in image from Uganda. Image processing was very complicated however the result surprised and amazed me - especially the visibility of very intricate coronal structures through rolling clouds. Moreover the image has some sort of beauty.

Click on the image or on the following reference to display the higher resolution image version (1.4 MB, PNG format).

ImageTse_2013_smh.png
Date3. 11. 2013
Time2nd contact 14:24:46 UT, Total eclipse duration 10 s (measured)
PlaceKenya
CoordinateN 3° 29' 42.07",   E 35° 26' 46.72",  Alt. 565 m
Conditionspartially cloudy
Optics(1) MTO 10/1000 mm
(2) 3M-5CA 8/500 mm
(3) 3M-65CA 6.3/500 mm
Camera(1,2,3) Canon EOS 5D Mark II (ISO 100)
Exposure(1) 1/250 s, 1/60 s,1/15 s
(2) 1/45 s, 1/15 s, 1/6 s
(3) 1/4 s, 1/1.4 s, 2 s
ProcessingComposition of 49 eclipse images - 23 images (1), 20 images (2), 6 images (3). Eclipse images were calibrated by means of large number of dark frames and flat-fields, aligned by means of phase correlation, composed by means of LDIC 5.0 software, processed using Corona 4.1 in order to visualize coronal structures. Final processing was done using ACC 6.1 software.
Image processing by Miloslav Druckmüller
SoftwareAstro D3F 2.0, PhaseCorr 6.0, LDIC 6.0, Corona 4.1, Sofo ACC 6.1
NoteThe graph above the table shows the average values of the relative number of sunspots in which the red line indicates the time of 2013 eclipse. Data from the World Data Center for the sunspot index, (Solar Influences Data Analysis Center, the Royal Observatory of Belgium) were used.
OrientationImage must be rotated 131° counter-clockwise to achieve standard orientation i. e. solar North up.
Copyright© 2013 Pavel Štarha, Kristián Molnár, Shadia Habbal   © 2014 Miloslav Druckmüller
 


Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
druckmuller@fme.vutbr.cz
Page last update: 28.7.2014