By L. Thomas (auth.), J. J. Burger, A. Pedersen, B. Battrick (eds.)
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Additional resources for Atmospheric Physics from Spacelab: Proceedings of the 11th ESLAB Symposium, Organized by the Space Science Department of the European Space Agency, Held at Frascati, Italy, 11–14 May 1976
Fig. DOMINGO interplanetary magnetic field. Apart from the frequency of disturbances that follow solar storms, no 11-year solar cycle has been found in the mean values of the solar wind parameters. e. ions and electrons accelerated to supratherma1 energies. Particles of relatively low energies are often released by the solar corona during periods extending over several solar rotations, thus producing the recurrent particle events with a period of 27 days. , electrons of several Mev and protons of more than I GeV are produced in association with large solar flares, as defined by the electromagnetic luminosity.
1974, 1975). The vorticity index is found to decrease by about 10% around the time when a sector boundary reaches the earth (Fig. 10). In the same line of research geomagnetic activity has been associated with troughs in the north pacific and with the thunderstorm activity (see review by Wilcox 1975). So far, in the lower atmosphere, we have reffered to periodical variations of local atmospheric parameter in the order of years and tens of years, limitations produced by the time of available good observations for the sensitivity involved.
Narcisi, in Physics and Chemistry of Upper Atmospherics, Ed. B. M. McCormac, Reidel, DordrechtHolland, 171, (1973). C. R. Detwiler, D. L. Garrett, J. D. Purcell and R. Tousey, Ann. Geophys. 17, 263, (1961). W. H. Parkinso~and E. M. Reeves, Solar Phys. 10, 342, (1969) • L. Heroux and R. A. Swirbalus, J. Geophys. Res. 81, 436, (1976). -A. B. Prag and F. A. Morse, J. Geophys. Res. 75, 4613, (1970). -= D. F. Heath, J. Geophys. Res. 78, 2779, (1973). H. E. Hinteregger, J. ~err. Phys. 38, (1976) (In Press).
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