Image

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).

ImageTse2010t_Ni_XV.png
Date11. 07. 2010
Time2nd contact 18:45:36 UT, 3rd contact 18:50:05 UT
Total eclipse duration 4 m 29 s
PlaceTatakoto Atoll, French Polynesia
CoordinateS 17° 20' 39.3'',   W 138° 27' 3.1'',  Alt. 6 m
ConditionsPartially clear, partially thin clouds
Optics2× 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
Camera2× Atik 314L+ (chip Sony ICX285AL)
ProcessingImage processing by Miloslav Druckmüller
SoftwarePhaseCorr 6.0, LDIC 5.0, Corona 4.1, Sofo ACC 6.1
NoteSee this ApJ paper for more details.
OrientationSee 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
 


Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
druckmuller@fme.vutbr.cz
Page last update: 6.8.2014