Abstract
The discussion of the development curves of several solar flares observed in the Hα-line leads to some new information about the photometric structure and behaviour of flares of importance from 1 to 2. The main results are as follows. An Hα-flare appears to be a pulsating phenomenon which, after an initial contraction, rapidly reaches its maximum and then exponentially grows fainter with time.
Analytical representations for both the pulsation periods and the exponential decreases are given. Many of the aspects of the flare phenomenon are more violent as the considered intensity level is higher.
A discussion on the present day state of solar patrol and some suggestions to improve it to be useful for solar physics is also made in the light of the present analysis.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Falciani, R., Righini, A., and Rigutti, M.: 1967, Z. Astrophys. 67, 481.
Falciani, R., Rigutti, M. and Macris, C. J.: 1972, Solar Phys., this issue, p. 108.
Reid, J. H.: 1971, IAU Coll., No. 11, ‘Automation in Optical Astrophysics’, Publ. Roy. Obs. Edinburgh 8, 1–211.
Severny, A. B.: 1964, Ann. Rev. Astron. Astrophys. 2, 363.
Smith, H. J. and Smith, E. v. P.: 1963, Solar Flares, MacMillan Co., New York.
Tandberg-Hanssen, E.: 1967, Solar Activity, Blaisdell Publ. Co., Waltham, Mass.
Zirin, H.: 1966, The Solar Atmosphere, Blaisdell Publ. Co., Waltham, Mass.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Falciani, R., Rigutti, M. Analysis of some aspects of 25 chromospheric events. Sol Phys 26, 114–129 (1972). https://doi.org/10.1007/BF00155112
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00155112