Imaging and spectroscopic observations of the 9 March 2016 Total Solar Eclipse in Palangkaraya

The March 9th 2016 total solar eclipse observation was carried out at Universitas Palangkaraya, Central Kalimantan. Time-resolved imaging of the Sun has been conducted before, after, and during totality of eclipse while optical spectroscopic observation has been carried out only at the totality. The...

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Bibliographic Details
Published in:Journal of physics. Conference series 2016-11, Vol.771 (1), p.12006
Main Authors: Kholish, Abdul Majid Al, Jihad, Imanul, Andika, Irham Taufik, Puspitaningrum, Evaria, Ainy, Fathin Q., Ramadhan, Sahlan, Arifyanto, M. Ikbal, Malasan, Hakim L.
Format: Article
Language:English
Subjects:
Cameras
Chromosphere
Diamonds
Emission analysis
Image resolution
Noise reduction
Physics
Signal processing
Signal to noise ratio
Solar corona
Solar eclipses
Spectra
Visual observation
White light
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Summary:The March 9th 2016 total solar eclipse observation was carried out at Universitas Palangkaraya, Central Kalimantan. Time-resolved imaging of the Sun has been conducted before, after, and during totality of eclipse while optical spectroscopic observation has been carried out only at the totality. The imaging observation in white light was done to take high resolution images of solar corona. The images were taken with a DSLR camera that is attached to a refractor telescope (d=66 mm, f 5.9). Despite cloudy weather during the eclipse moments, we managed to obtain the images with lower signal-to-noise ratio, including identifiable diamond ring, prominence and coronal structure. The images were processed using standard reduction procedure to increase the signal-to-noise ratio and to enhance the corona. Then, the coronal structure is determined and compared with ultraviolet data from SOHO to analyze the correlation between visual and ultraviolet corona. The spectroscopic observation was conducted using a slit-less spectrograph and a DSLR camera to obtain solar flash spectra. The flash spectra taken during the eclipse show emissions of H 4861 Å, He I 5876 Å, and H 6563 Å. The Fe XIV 5303 Å and Fe X 6374 Å lines are hardly detected due to low signal-to-noise ratio. Spectral reduction and analysis are conducted to derive the emission lines intensity relative to continuum intensity. We use the measured parameters to determine the temperature of solar chromosphere.
ISSN:1742-6588
1742-6596
DOI:10.1088/1742-6596/771/1/012006