Simulation of the anomalous cosmic ray radiation belt with atmospheric production and decay

2001 ◽  
Vol 28 (17) ◽  
pp. 3417-3420 ◽  
Author(s):  
R. S. Selesnick
Keyword(s):  
Radiation Belt ◽  
Cosmic Ray

scholarly journals A radiation belt of energetic protons located between Saturn and its rings

Science ◽  
2018 ◽  
Vol 362 (6410) ◽  
pp. eaat1962 ◽  
Author(s):  
E. Roussos ◽  
P. Kollmann ◽  
N. Krupp ◽  
A. Kotova ◽  
L. Regoli ◽  
...  
Keyword(s):  
Radiation Belt ◽  
Cosmic Ray ◽  
High Energy ◽  
Radiation Belts ◽  
Exchange Reactions ◽  
Dipole Magnetic Field ◽  
Imaging Instrument ◽  
Multiple Charge ◽  
Strong Dipole ◽  
Dense Atmosphere

Saturn has a sufficiently strong dipole magnetic field to trap high-energy charged particles and form radiation belts, which have been observed outside its rings. Whether stable radiation belts exist near the planet and inward of the rings was previously unknown. The Cassini spacecraft’s Magnetosphere Imaging Instrument obtained measurements of a radiation belt that lies just above Saturn’s dense atmosphere and is decoupled from the rest of the magnetosphere by the planet’s A- to C-rings. The belt extends across the D-ring and comprises protons produced through cosmic ray albedo neutron decay and multiple charge-exchange reactions. These protons are lost to atmospheric neutrals and D-ring dust. Strong proton depletions that map onto features on the D-ring indicate a highly structured and diverse dust environment near Saturn.

Post-storm cosmic ray increases and the radiation belt

1965 ◽  
Vol 27 (5) ◽  
pp. 635-640 ◽  
Author(s):  
J.N. Tandon ◽  
V.B. Bhatia
Keyword(s):  
Radiation Belt ◽  
Cosmic Ray

COSMIC-RAY ANTIPROTON SPATIAL DISTRIBUTIONS COMPUTED IN MAGNETOSPHERE

2005 ◽  
Vol 20 (29) ◽  
pp. 6739-6741 ◽  
Author(s):  
MICHIO FUKI
Keyword(s):  
Radiation Belt ◽  
Polar Region ◽  
Initial Conditions ◽  
Outer Region ◽  
Cosmic Ray ◽  
Spatial Distributions ◽  
Cosmic Ray Interactions ◽  
Arrival Directions

The motion of antiprotons in the Magnetosphere region is computed with some initial conditions and the spatial distributions of them are plotted. The antiprotons in the polar region are looked like coming from the outer region. Meanwhile, the antiprotons on the ISS altitude are trapped in the radiation belt. This is explained by the model that antiprotons are originated in decay particles from the antineutrons produced with the cosmic ray interactions in the atmosphere. This also shows that they are rich in the SAA region in the ISS altitudes. In order to distinguish antiprotons from protons effectively, the differences of arrival directions of them are important.

"Radiation Belt" and Trapped Cosmic-Ray Albedo

1958 ◽  
Vol 1 (5) ◽  
pp. 171-173 ◽  
Author(s):  
S. F. Singer
Keyword(s):  
Radiation Belt ◽  
Cosmic Ray

International workshop on new standard radiation belt and plasma models

Space Weather ◽  
2005 ◽  
Vol 3 (2) ◽  
pp. n/a-n/a
Author(s):  
Jean-Marie Lauenstein
Keyword(s):  
Radiation Belt ◽  
International Workshop

DEVELOPMENT OF THE COSMIC RAY TECHNIQUES

1982 ◽  
Vol 43 (C8) ◽  
pp. C8-69-C8-88 ◽  
Author(s):  
B. Rossi
Keyword(s):  
Cosmic Ray

Cosmic ray variations and space weather

2010 ◽  
Vol 180 (5) ◽  
pp. 519 ◽  
Author(s):  
L.I. Dorman
Keyword(s):  
Space Weather ◽  
Cosmic Ray
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