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V. (1975): Wavesand instabil ities phys. , Vol. 13, 263. in the solar wind. 3O Copyright American Geophysical Union Rev. Geo- Special Publications Physics of Solar Planetary Environments: Proceedings of the International Symposium on Solar-Terrestrial Physics June 7–18,1976, Boulder, Colorado, Volume I Vol. 7 Hundhausen, A. J. (1972): CoronalExpansionand Solar Wind. Springer-Verlag, New York. Jacchia, L. G. (1976): Private communication. Jacchia, L. , J. W. Sloweyand I. G. Campbell(1973). Ananalysis of the solar-activity effects in the upperatmosphere.
Solar Phys. 32:389. Howard, R. (1974a): Studiesof solar magnetic fields,II: The magnetic fluxes. Solar Phys. 38:59. Howard, R. (1974b): Studies of solar magnetic fields, I: The average field strengths. Solar Phys. 38:283. Kopeck•,M. (1970): Babcock's theoryof the 22-year solar cycleandthelatitude drift of thesunspot zone. _andA_srroph),s. 7:57. Leighton, R. B. (1964): Transport of magnetic fields on the sun. Astrophys. J. 140:1547. 42 Copyright American Geophysical Union Vol. 7 Special Publications Physics of Solar Planetary Environments: Proceedings of the International Symposium on Solar-Terrestrial Physics June 7–18,1976, Boulder, Colorado, Volume I Leighton,R.
7 and with Like other solar-terrestrial phenomena, the next step should be to find physical parameters or physical quantities which control the correIn the early part of this paper, we learned how difficult it is to find such a parameter for geomagneticdisturbances, which have finally been identified to be the north-south 8. component of the interplanetary magnetic field. SUMMARY We have now established the basic solar-interplanetary magnetic field structure, together with the associated solar wind structures.