The influences of solar wind pressure and interplanetary magnetic field on global magnetic field and outer radiation belt electrons

Using the Van Allen Probe in situ measured magnetic field and electron data, we examine the solar wind dynamic pressure and interplanetary magnetic field (IMF) effects on global magnetic field and outer radiation belt relativistic electrons (≥1.8 MeV). The dynamic pressure enhancements (>2 nPa) c...

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Bibliographic Details
Published in:Geophysical research letters 2016-07, Vol.43 (14), p.7319-7327
Main Authors: Yu, J., Li, L.Y., Cao, J. B., Reeves, G. D., Baker, D. N., Spence, H.
Format: Article
Language:English
Subjects:
Anisotropy
Asymmetry
Butterflies
butterfly distributions
Compressing
Compression
day‐night asymmetrical variations of magnetic field
day‐night asymmetrical variations of relativistic electron pitch angle distributions
Drift
Dynamic pressure
Electron energy
Energy
Flux
GEOSCIENCES
Heliospheric and Magnetospheric Physics
Interplanetary magnetic field
Interplanetary magnetic fields
Magnetic field
Magnetic fields
Magnetism
Magnetopause
Night
Night-time
Nighttime
Outer radiation belt
pancake distributions
Pressure
Radiation
Radiation belt electrons
Reduction
Relativism
Shadows
Solar wind
solar wind dynamic pressure
southward interplanetary magnetic field
Spatial distribution
Splitting
Stress concentration
Wind pressure
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Summary:Using the Van Allen Probe in situ measured magnetic field and electron data, we examine the solar wind dynamic pressure and interplanetary magnetic field (IMF) effects on global magnetic field and outer radiation belt relativistic electrons (≥1.8 MeV). The dynamic pressure enhancements (>2 nPa) cause the dayside magnetic field increase and the nightside magnetic field reduction, whereas the large southward IMFs (Bz‐IMF  4), the pitch angles of relativistic electrons are mainly pancake distributions with a flux peak around 90° (corresponding anisotropic index A > 0.1), and the higher‐energy electrons have stronger pancake distributions (the larger A), suggesting that the compression‐induced betatron accelerations enhance the dayside pancake distributions. However, in the nighttime decreased magnetic field region (MLT ~ 18:00–06:00, and L ≥ 5), the pitch angles of relativistic electrons become butterfly distributions with two flux peaks around 45° and 135° (A 
ISSN:0094-8276
1944-8007
DOI:10.1002/2016GL069029