Dynamics of the low altitude secondary proton radiation belt.
At the interface between the upper atmosphere and the radiation belt region, there exists a secondary radiation belt consisting mainly of energetic ions that have become neutralized in the ring current and the main radiation belt and then re-ionized by collisions in the inner exosphere. The time history of the proton fluxes in the 0.64-35 MeV energy range was traced in the equatorial region beneath the main radiation belts during the three year period from 21 February 1984 to 26 March 1987 using data obtained with the HEP experiment on board the Japanese OHZORA satellite. During most of this period a fairly small proton flux of -1.2 cm-2 S-1 sr-1 was detected on geomagnetic field lines in the range 1.05 < L < 1.15. We report a few surprisingly deep and rapid flux decreases (flux reduction by typically two orders of magnitude). These flux decreases were also long in duration (lasting up to three months). We also registered abrupt flux increases where the magnitude of the proton flux enhancements could reach three orders of magnitude with an enhancement duration of 1-3 days. Possible reasons for these unexpected phenomena are discussed.
Gusev
A A
AA
University of Campinas, Depto. de Raios Cosmicos, Brazil.
Kohno
T
T
Spjeldvik
W N
WN
Martin
I M
IM
Pugacheva
G I
GI
Turtelli
A
A
D001272:Atmosphere / Q000032:analysis; D018534:Earth, Planet; D005118:Extraterrestrial Environment; D008280:Magnetics; D011522:Protons; D011834:Radiation Monitoring / Q000295:instrumentation*; D013026:Space Flight / Q000295:instrumentation*; D018531:Spacecraft / Q000295:instrumentation*
D011522:Protons