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Title: Proposed visible emission line space solar coronagraph
Authors: Singh, J
Prasad, B. R
Venkatakrishnan, P
Sankarasubramanian, K
Banerjee, D
Bayanna, R
Mathew, S
Murthy, J
Subramaniam, P
Ramesh, R
Kathiravan, S
Nagabhushana, S
Mahesh, P. K
Manoharan, P. K
Uddin, W
Sriram, S
Amit Kumar
Srivastava, N
Koteswara Rao
Nagendra, C. L
Chakraborty, P
Sriram, K. V
Venkateswaran, R
Krishnamurthy, T
Sreekumar, P
Sarma, K. S
Murthy, R
Navalgund, K. H
Samudraiah, D. R. M
Narayan Babu, P
Patra, A
Keywords: Coronal mass ejection;Payload;Solar coronagraph;Spectral window
Issue Date: 25-Jan-2011
Publisher: Indian Academy of Sciences
Citation: Current Science, Vol. 100, No. 2, pp. 167-174
Abstract: The outer atmosphere of the sun – called the corona – has been observed during total solar eclipse for short periods (typically < 6 min), from as early as the eighteenth century. In the recent past, space-based instruments have permitted us to study the corona uninterruptedly. In spite of these developments, the dynamic corona and its high temperature (1–2 million K) are yet to be fully understood. It is conjectured that their dynamic nature and associated energetic events are possible reasons behind the high temperature. In order to study these in detail, a visible emission line space solar coronagraph is being proposed as a payload under the small-satellite programme of the Indian Space Research Organisation. The satellite is named as Aditya-1 and the scientific objectives of this payload are to study: (i) the existence of intensity oscillations for the study of wavedriven coronal heating; (ii) the dynamics and formation of coronal loops and temperature structure of the coronal features; (iii) the origin, cause and acceleration of coronal mass ejections (CMEs) and other solar active features, and (iv) coronal magnetic field topology and three-dimensional structures of CMEs using polarization information. The uniqueness of this payload compared to previously flown space instruments is as follows: (a) observations in the visible wavelength closer to the disk (down to 1.05 solar radii); (b) high time cadence capability (better than two-images per second), and (c) simultaneous observations of at least two spectral windows all the time and three spectral windows for short durations.
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