Abstract
Isophotes obtained by equidensitometry techniques from four exposures of the March 7, 1970 corona are used for derivation of intensity distributions along the equator, poles, streamers and dark ‘gaps’ in the visible corona. The distributions differ from the van de Hulst curves for a maximum corona. The Kodaikanal measures agree well with the NRL measures of the outer corona made from a rocket coronagraph and together provide data from 1·2R⊙ to 8·0R⊙ along the solar equator. Radial intensity gradients for different position angles and the Ludendorff parameters obtained, characterize this corona as typical of the solar maximum.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Bappu M K V and Bhatnagar A 1967Kodaikand Observe. Bull. Ser. A No. 190
Bappu M K V, Bhattacharyya J C and Sivaraman K R 1972Solar Phys. 26 366
Baumbach S 1937Astron. Nachr. 263 121
Becker L 1908Mem. Roy. Astron. Soc. 57 307
Bohlin J D, Koomen M J and Tousey R 1971Solar Phys.,21 408
Gulyaev R A 1971Russian Solar Data No. 6 p 80
van de Hulst H C 1950Bull. Astron. Inst. Neth. 11 135
Waldmeier M 1970Nature, London 226 1139
Waldmeier M 1971Physics of the Solar Corona (Reidel Publ. Co., Dordrecht-Holland) p. 130
Wallenquist A 1956Ann. Observe. Uppsala,4 No. 4
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Bappu, M.K.V., Bhattacharyya, J.C. & Sivaraman, K.R. Photometry of the solar corona of March 7, 1970. Pramana - J Phys 1, 117–128 (1973). https://doi.org/10.1007/BF02846657
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF02846657