Data processing of Visible Emission Line Coronagraph Onboard ADITYA L1

ADITYA-L1 is India's first dedicated mission to observe the sun and its atmosphere from a halo orbit around L1 point. Visible emission line coronagraph (VELC) is the prime payload on board at Aditya-L1 to observe the sun's corona. VELC is designed as an internally occulted reflective coron...

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Published in:arXiv.org 2023-07
Main Authors: Priyal, Muthu, Singh, Jagdev, B Raghavendra Prasad, Chavali Sumana, Kumar, Varun, Mishra, Shalabh, Venkata, S N, Sindhuja, G, K Sasikumar Raja, Kumar, Amit, krishnan, Sanal, Hegde, Bhavana S, Utkarsha, D, Venkatasubramanian, Natarajan, Somasundram, Pawankumar, Nagabhushana, S, Kamath, PU, Kathiravan, S, Mani, T Vishnu, Basavaraju, Suresh, Chavan, Rajkumar, Vemareddy, P, Ravindra, B, Rajaguru, S P, Nagaraju, K, Mishra, Wageesh, Joshi, Jayant, Samanta, Tanmoy, Chatterjee, Piyali, Kathiravan, C, Ramesh, R
Format: Article
Language:English
Subjects:
Algorithms
Calibration
Coronagraphs
Data processing
Detectors
Emission spectra
Image processing
Lagrangian equilibrium points
Line spectra
Physical properties
Software
Solar corona
Solar limb
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Summary:ADITYA-L1 is India's first dedicated mission to observe the sun and its atmosphere from a halo orbit around L1 point. Visible emission line coronagraph (VELC) is the prime payload on board at Aditya-L1 to observe the sun's corona. VELC is designed as an internally occulted reflective coronagraph to meet the observational requirements of wide wavelength band and close to the solar limb (1.05 Ro). Images of the solar corona in continuum and spectra in three emission lines 5303Å [Fe xiv], 7892Å [Fe xi] and 10747 [Fe xiii] obtained with high cadence to be analyzed using software algorithms automatically. A reasonable part of observations will be made in synoptic mode, those, need to be analyzed and results made available for public use. The procedure involves the calibration of instrument and detectors, converting the images into fits format, correcting the images and spectra for the instrumental effects, align the images etc. Then, develop image processing algorithms to detect the occurrence of energetic events using continuum images. Also derive physical parameters, such as temperature and velocity structure of solar corona using emission line observations. Here, we describe the calibration of detectors and the development of software algorithms to detect the occurrence of CMEs and analyze the spectroscopic data.
ISSN:2331-8422