Ni XV, 670.2 nm
Ni XV is very weak line mainly due to a factor of 20 lower nickel abundance in solar corona compared
to iron. Image calibration and processing must be very precise in order to separate the emission line
from continuum (photospheric light scattered on free electrons).
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Image | Tse2010t_Ni_XV.png |
Date | 11. 07. 2010 |
Time | 2nd contact 18:45:36 UT, 3rd contact 18:50:05 UT Total eclipse duration 4 m 29 s |
Place | Tatakoto Atoll, French Polynesia |
Coordinate | S 17° 20' 39.3'', W 138° 27' 3.1'', Alt. 6 m |
Conditions | Partially clear, partially thin clouds |
Optics | 2× Thorlabs near IR achromat 4/200mm equipped with following narrow band filters: On-band filter: Andover, center wavelenght: 670.2 nm, bandwidth 50%: 0.5 nm Off-band filter: Andover, center wavelenght: 669.1 nm, bandwidth 50%: 0.5 nm |
Camera | 2× Atik 314L+ (chip Sony ICX285AL) |
Processing | Image processing by Miloslav Druckmüller |
Software | PhaseCorr 6.0, LDIC 5.0, Corona 4.1, Sofo ACC 6.1 |
Note | See this ApJ paper for more details. |
Orientation | See this image. The white circle represents the position of photosphere. |
Copyright | © 2010 Shadia Habbal, Huw Morgan, Judd Johnson, Martina Arndt, Adrian Daw © 2011 Miloslav Druckmüller |
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Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
druckmuller@fme.vutbr.cz
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Page last update: 27.11.2019
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