Fe XIV emission on/off line animation

This animation illustrates that even though the filter used for Fe XIV emission photography was of 0.15 nm bandwidth, the contamination of the image by continuum is still very high. Both images (530.2 nm on-line, 529.1 nm off-line) are in logarithm brightness scala and without any structure enhancement. The images were precisely calibrated therefore any change in brightness you see in the animation is caused by a change of radiation intensity and not by difference of brightness scala. The change of brightness is only minor in polar regions where the Fe XIV emission is very weak. A strong Fe XIV emission is clearly visible in active regions as a significant brightness change.

Date01. 08. 2008
Time2nd contact 11:03:35 UT, 3rd contact 11:05:39 UT
Total eclipse duration 2 m 4 s
PlaceMongolia, Bor Udzuur
Coordinate45° 43.251' N, 92° 06.837' E, 1223 m altitude
ConditionsExcellent - clear sky, altitude of the Sun above the horizon 22°
Opticson-line: Beroflex 8/500mm, 530.2nm filter, bandwidth 0.15nm (Andover Corp. USA)
off-line: Exakta 8/500mm, 529.1nm filter, bandwidth 0.15nm (Andover Corp. USA)
Cameratwo Canon EOS 5D cameras
Exposure1 s - 8 s (ISO 400), 8 s (ISO 800), 8 s (ISO 1600)
Processing12 on-line and 12 off-line images were used. Eclipse images were calibrated by means of dark frames and flat-fields, aligned by means of phase correlation then composed by means of LDIC 5.0 software.
Image processing by Miloslav Druckmüller
SoftwareAstro D3F 2.0, PhaseCorr 6.0, LDIC 5.0, Corona 4.1, Sofo ACC 6.1
OrientationImage must be rotated 8.3° clockwise to achieve standard orientation i. e. North up.
Copyright© 2008 Miloslav Druckmüller, Vojtech Rušin, Ľubomír Klocok, Peter Aniol, Karel Martišek

Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
Page last update: 9.10.2009