: k S u b m i t t e d t o J o u r n a l of Geophysical R e s e a r c h , J u l y 27, 1965. f . ... e a d s t o r a p i d diffusion and p a r t i c l e l o s s , t h e r e q u i r e m e n t t h a t the g r o w t h rate be l i m i t e d t o the rate a t which wave e n e r g y is depleted by wave p r o p a g a t i o n allows a n e s t i m a t e of a n u p p e r l i m i t t o the t r a p p e d e q u a t o r i a l p a r t i c l e flux.E l e c t r o n f l u x e s > 40 keV and proton fluxes > 120 keV o b s e r v e d on E x p l o r e r s XIV and XI1 r e s p e c t i v e l y obey t h i s limit with o c c a s i o n a l exceptions. L = 4, a c c e l e r a t i o n s o u r c e sufficient t o keep t h e t r a p p e d p a r t i c l e s n e a r t h e i r p r e c i p it a t i o n l i m i t e x i s t s .s u g g e s t i n g a p a r t i a l explanation f o r the e x i s t e n c e of l a r g e r d e n s i t i e s of high e n e r g y p r o t o n s than e l e c t r o n s .pond t o a diffusion coefficient in a g r e e m e n t with o b s e r v e d l i f e t i m e s . q u i r e d e q u a t o r i a l w h i s t l e r mode wide band n o i s e intensity, obviously i n c o n s i s t e n t with o b s e r v a t i o n s , and is c o n s i s t e n t with t h e l i f e t i m e

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The Chapman and Ferraro [e.g., Beard, 1960] model of the magnetosphere is entirely dissipationless and, as a consequence, contains no tangential stress at the magnetosphere boundary. It has been suggested that either viscous interaction [Axford and Hines, 1961; Piddington, 1963] or reconnection of field lines [Dungey, 1961; Levy, Petschek, and Siscoe, 1963] can give rise to tangential stresses which produce internal convection within the magnetosphere. A number of auroral and ionospheric observations appear to be consistent with such a convection pattern. It was also suggested [Piddington, 1960] that tangential stresses might stretch the magnetosphere tail and thus account for the main phase of magnetic storms.

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