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STOCHASTIC ACCELERATION OF COSMIC RAYS IN ANISOTROPIC PLASMA TURBULENCE. Yurij Fedorov 1 , and Milan Stehlik 2 1 Main Astronomical Observatory NASU, Kiev, Ukraine 2 Institute of Experimental Physics SAS, Ko š ice, Slovakia. The diffusion coefficient in momentum space. Conclusions. - PowerPoint PPT Presentation
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STOCHASTIC ACCELERATION OF COSMIC RAYS IN STOCHASTIC ACCELERATION OF COSMIC RAYS IN ANISOTROPIC PLASMA TURBULENCEANISOTROPIC PLASMA TURBULENCE
Yurij FedorovYurij Fedorov11, and Milan Stehlik, and Milan Stehlik22
1Main Astronomical Observatory NASU, Kiev, Ukraine2Institute of Experimental Physics SAS, Košice, Slovakia
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The diffusion coefficient in momentum spaceThe diffusion coefficient in momentum space
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F ig .4 . T h e e n e rg e t ic s p e c tra c o r re s p o n d in g to th e s te a d y s ta te s o lu t io n (1 1 ) ,(1 2 ) .
N u m b e rs n e a r c u rv e s c o r re s p o n d to d im e n s io n le s s p a ra m e te r e = t e / t 0 .
T h e m o m e n tu m d if fu s io n c o e f f ic ie n t is g iv e n b y e q u a t io n (5 ) ; = 0 .5 .
1 0 -1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 4
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F ig .5 . T h e e n e r g e t ic s p e c t r a c o r r e s p o n d in g to th e s te a d y s ta te s o lu t io n ( 1 1 ) ,( 1 2 ) .
N u m b e r s n e a r c u r v e s c o r r e s p o n d to d im e n s io n le s s p a r a m e te r e = t e / t 0 .
T h e m o m e n tu m d i f f u s io n c o e f f ic ie n t i s g iv e n b y e q u a t io n ( 6 ) ; = 0 .5 .
1 0-1
1 00
1 01
1 02
1 03
1 04
1 0-8
1 0-7
1 0-6
1 0-5
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Fig.7. The differential proton spectra on June 15, 1991 GLE
(Belov, Eroshenko, 1996).
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F ig .9 . T h e sp ec tra o f en erg e tic p a rtic les u n d er m o n o en erg e tic in jec tio n .
N u m b er n ea r cu rv es d en o te d im en sio n less tim e; D p = D F ; = 0 .5 .
10-1
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F ig .1 0 . T h e s p e c tra o f e n e rg e t ic p a r t ic le s u n d e r m o n o e n e rg e t ic in je c t io n .
N u m b e r n e a r c u rv e s d e n o te d im e n s io n le s s t im e ; D p = D k ; = 0 .5 .
1 0-1
1 00
1 01
1 02
1 03
1 0-6
1 0-5
1 0-4
1 0-3
1 0-2
1 0-1
1 00
S te a d y s ta te s o lu t io n
0 .20 .0 50 .0 10 .0 0 1N m c2/q t
0
Ek, M e V
ConclusionsConclusions
Particle acceleration by large scale EF can Particle acceleration by large scale EF can be efficient for a medium of sufficiently be efficient for a medium of sufficiently high magnetic helicityhigh magnetic helicity
The results can be useful for description of The results can be useful for description of particle acceleration in astrophysical particle acceleration in astrophysical objects ( solar flares, supernova remnants, objects ( solar flares, supernova remnants, galactic nuclei, … )galactic nuclei, … )
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