Solar-Cycle Variations of Invariant Parameters of Ion Energy Spectra of the Earths Radiation Belts

Analyzing the data from the satellites Injun-4, Injun-5, 1968-26B, OVI-19, Explorer-45, 1972-076B, Molniya-I, ATS-6, Molniya-2, Geos-i, Geos-2, ISEE-I, SCATHA, AMPTE/CCE, Gorizont-21, Viking, Akebono, CRRES, Gorizont-25, and ETS-VI (1965-1994) by the method of "a spectrometer with a magnetic sail" we have found, for a region of adiabatic transport of particles in a geomagnetic trap, the invariant parameters of steady-state distributions of ions H+, He+, He2+, and [CNO] group (charges from +1 up to +6) over the orbital magnetic moment (mo) in the range 0.01-50 keV/nT. These distributions are shown to vary with the 11-year solar activity cycle. The spectra have a maximum at (mo(m) 0.5 ± 0.2 keV/nT, the exponential form with the index (mo)o(xi) = 0.3 ± 0.2 keV/nT at (mo)m/(xi)<(mo)/(xi)<(mo)b/(xi), a power-law tail with the exponent (gamma) = 4.7 ± 2.2 at (mo)/(xi)>(mo)b/(xi) = 1.4± 0.8 keV/nT, with (mo)b = (gamma)(mo)o and, usually,(mo)m#(mo)o. 11(3. Between the minimum and maximum of solar activity, a coefficient of spectra similarity, (xi), varies from M(i) to Q(i) (M(i) and Q(i) are the mass and charge of ions in terms of appropriate proton parameters); the exponential segment of spectra steepens (mo/xi) decreases by a factor of 1.5-2); the parameter(mo)b/xi) increases, however (mo(b)) varies insignificantly; the indices (gamma) of power-law tails of various ion components approximately coincide and respond to solar activity much more weakly than to substorms.