Abstract
The phenomenon of a difference between solar EVV fluxesI λ (λ<130 nm) measured for the same solar indices but in cycles of different amplitudes is studied. The difference can reach 15–20%. The phenomenon is explained in terms of a two-component model of solar EUV variations (from the active regions and the “undisturbed” solar surface). It follows from this model that in powerful cycles the fluxesI λ must be greater than in weak cycles for the same solar index F10.7. The results of the HI α line measurements from SME are presented as an example of the possibility of solar cycle amplitude prediction about two years before the solar maximum epoch.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
V. V. Katyushina, M. V. Krasinets, A. A. Nusinov, Ch. A. Bart, and G. Zh. Rottman,Geomagn. Aéronom.,31, No. 1, 40 (1991).
A. Vidal-Madjar and B. Pissamay,Sol. Phys.,66, No. 2, 259 (1980).
A. Vidal-Madjar, C. Emerich, and S. Cazes,Astron. Astrophys.,87, No. 3, L12 (1980).
Solar Geophysical Data (prompt reports), NOAA, USA (1982–1990).
Author information
Authors and Affiliations
Additional information
Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 39, No. 10, pp. 1237–1241, October, 1996.
Rights and permissions
About this article
Cite this article
Nusinov, A.A. Hysteresis of a solar EUV flux and the relation of its characteristics to the solar cycle amplitude. Radiophys Quantum Electron 39, 830–832 (1996). https://doi.org/10.1007/BF02120967
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF02120967