Abstract
The X-ray emission of individual solar active regions is found from OSO-5 data to vary on three main timescales. Flare associated events typically last for times of minutes to an hour. Events lasting several hours, with several peaks in the X-ray emission, are accompanied by a simplification in the magnetic field, and often mark a turning point in the life of the region. Smooth changes over periods of several days are associated with the general development of a region. Examples of these last two variations are presented.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Bruzek, A.: 1967, Solar Phys. 2, 451.
Bruzek, A.: 1969, Solar Phys. 8, 29.
Culhane, J. L. and Phillips, K. J. H.: 1970, Solar Phys. 11, 117.
Drake, J. F.: 1970, Thesis, University of Iowa.
Herring, J. R. H., Glencross, W. M., Parkinson, J. H., and Pounds, K. A.: 1971, Proc. Roy. Soc. London A321, 493.
Kane, S.: 1971, Private communication.
Krieger, A., Paolini, F., Vaiana, G. D., and Webb, D.: 1972, Solar Phys. 22, 150.
Moreton, G. E.: 1960, Astron. J. 65, 494.
Moreton, G. E.: 1964, Astron. J. 69, 145.
Parkinson, J. H.: 1973, Solar Phys. 28, 487.
Parkinson, J. H. and Pounds, K. A.: 1971, Solar Phys. 17, 146.
Teske, R. G.: 1969, Solar Phys. 6, 193.
Weart, S. R. and Zirin, H.: 1969, Publ. Astron. Soc. Pac. 81, 270.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Parkinson, J.H. Time variations in the X-ray emission of solar active regions. Sol Phys 28, 137–150 (1973). https://doi.org/10.1007/BF00152918
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00152918