Ring current ions and radiation belt electrons during geomagnetic storms driven by coronal mass ejections and corotating interaction regions

2005 ◽  
Vol 32 (21) ◽  
Author(s):  
Yoshizumi Miyoshi ◽  
Ryuho Kataoka
Keyword(s):  
Coronal Mass Ejections ◽  
Radiation Belt ◽  
Ring Current ◽  
Geomagnetic Storms ◽  
Corotating Interaction Regions ◽  
Radiation Belt Electrons ◽  
Interaction Regions

scholarly journals Magnetospheric Response to Solar Wind Forcing: ULF Wave – Particle Interaction Perspective

2021 ◽  
Author(s):  
Qiugang Zong
Keyword(s):  
Solar Wind ◽  
Radiation Belt ◽  
Ring Current ◽  
Dynamic Pressure ◽  
Plasma Heating ◽  
Interplanetary Shock ◽  
Wind Forcing ◽  
Ulf Waves ◽  
Radiation Belt Electrons ◽  
The Impact

Abstract. Solar wind forcing, e.g. interplanetary shock and/or solar wind dynamic pressure pulses impact on the Earth’s magnetosphere manifests many fundamental important space physics phenomena including producing electromagnetic waves, plasma heating and energetic particle acceleration. This paper summarizes our present understanding of the magnetospheric response to solar wind forcing in the aspects of radiation belt electrons, ring current ions and plasmaspheric plasma physics based on in situ spacecraft measurements, ground-based magnetometer data, MHD and kinetic simulations. Magnetosphere response to solar wind forcing, is not just a “one-kick” scenario. It is found that after the impact of solar wind forcing on the Earth’s magnetosphere, plasma heating and energetic particle acceleration started nearly immediately and could last for a few hours. Even a small dynamic pressure change of interplanetary shock or solar wind pressure pulse can play a non-negligible role in magnetospheric physics. The impact leads to generate series kind of waves including poloidal mode ultra-low frequency (ULF) waves. The fast acceleration of energetic electrons in the radiation belt and energetic ions in the ring current region response to the impact usually contains two contributing steps: (1) the initial adiabatic acceleration due to the magnetospheric compression; (2) followed by the wave-particle resonant acceleration dominated by global or localized poloidal ULF waves excited at various L-shells. Generalized theory of drift and drift-bounce resonance with growth or decay localized ULF waves has been developed to explain in situ spacecraft observations. The wave related observational features like distorted energy spectrum, boomerang and fishbone pitch angle distributions of radiation belt electrons, ring current ions and plasmaspheric plasma can be explained in the frame work of this generalized theory. It is worthy to point out here that poloidal ULF waves are much more efficient to accelerate and modulate electrons (fundamental mode) in the radiation belt and charged ions (second harmonic) in the ring current region. The results presented in this paper can be widely used in solar wind interacting with other planets such as Mercury, Jupiter, Saturn, Uranus and Neptune, and other astrophysical objects with magnetic fields.

scholarly journals Simultaneous observations of precipitating radiation belt electrons and ring current ions associated with the plasmaspheric plume

2013 ◽  
Vol 118 (7) ◽  
pp. 4391-4399 ◽  
Author(s):  
Zhigang Yuan ◽  
Ming Li ◽  
Ying Xiong ◽  
Haimeng Li ◽  
Meng Zhou ◽  
...  
Keyword(s):  
Radiation Belt ◽  
Ring Current ◽  
Radiation Belt Electrons

scholarly journals Evolution of the outer radiation belt during the November 1993 storms driven by corotating interaction regions

2007 ◽  
Vol 112 (A5) ◽  
pp. n/a-n/a ◽  
Author(s):  
Y. Miyoshi ◽  
A. Morioka ◽  
R. Kataoka ◽  
Y. Kasahara ◽  
T. Mukai
Keyword(s):  
Radiation Belt ◽  
Outer Radiation Belt ◽  
Corotating Interaction Regions ◽  
Interaction Regions

Major geomagnetic storms (Dst≤ −100 nT) generated by corotating interaction regions

2006 ◽  
Vol 111 (A7) ◽  
Author(s):  
I. G. Richardson ◽  
D. F. Webb ◽  
J. Zhang ◽  
D. B. Berdichevsky ◽  
D. A. Biesecker ◽  
...  
Keyword(s):  
Geomagnetic Storms ◽  
Corotating Interaction Regions ◽  
Interaction Regions
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