Shock acceleration of energetic particles in corotating interaction regions in the solar wind

1980 ◽  
Vol 237 ◽  
pp. 620 ◽  
Author(s):  
L. A. Fisk ◽  
M. A. Lee
Keyword(s):  
Solar Wind ◽  
Energetic Particles ◽  
Shock Acceleration ◽  
Corotating Interaction Regions ◽  
Interaction Regions

scholarly journals Modeling transport of energetic particles in corotating interaction regions: A case study

2016 ◽  
Vol 121 (1) ◽  
pp. 77-92 ◽  
Author(s):  
Lulu Zhao ◽  
Gang Li ◽  
R. W. Ebert ◽  
M. A. Dayeh ◽  
M. I. Desai ◽  
...  
Keyword(s):  
Energetic Particles ◽  
Corotating Interaction Regions ◽  
Modeling Transport ◽  
Interaction Regions

scholarly journals STEREO and ACE Observations of Energetic Particles from Corotating Interaction Regions

2010 ◽  
Author(s):  
R. A. Leske ◽  
R. A. Mewaldt ◽  
G. M. Mason ◽  
C. M. S. Cohen ◽  
A. C. Cummings ◽  
...  
Keyword(s):  
Energetic Particles ◽  
Corotating Interaction Regions ◽  
Interaction Regions

scholarly journals Solar wind interaction with comet 67P: Impacts of corotating interaction regions

2016 ◽  
Vol 121 (2) ◽  
pp. 949-965 ◽  
Author(s):  
N. J. T. Edberg ◽  
A. I. Eriksson ◽  
E. Odelstad ◽  
E. Vigren ◽  
D. J. Andrews ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction ◽  
Corotating Interaction Regions ◽  
Interaction Regions ◽  
Comet 67P

Solar wind flow angle and geoeffectiveness of corotating interaction regions: First results

2017 ◽  
Vol 44 (10) ◽  
pp. 4532-4539 ◽  
Author(s):  
Diptiranjan Rout ◽  
D. Chakrabarty ◽  
P. Janardhan ◽  
R. Sekar ◽  
Vrunda Maniya ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Corotating Interaction Regions ◽  
Flow Angle ◽  
First Results ◽  
Solar Wind Flow ◽  
Interaction Regions

scholarly journals Solar Wind ∼0.15–1.5 keV Electrons around Corotating Interaction Regions at 1 au

2021 ◽  
Vol 922 (2) ◽  
pp. 198
Author(s):  
Jiawei Tao ◽  
Linghua Wang ◽  
Gang Li ◽  
Robert F. Wimmer-Schweingruber ◽  
Chadi Salem ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Speed ◽  
Kinetic Temperature ◽  
Number Density ◽  
Kappa Index ◽  
Corotating Interaction Regions ◽  
Fast Wind ◽  
Magnetic Field Magnitude ◽  
Interaction Regions ◽  
The Relationship

Abstract Here we present a statistical study of the ∼0.15–1.5 keV suprathermal electrons observed in uncompressed/compressed slow and fast solar wind around 59 corotating interaction regions (CIRs) with good measurements by Wind 3DP from 1995 through 1997. For each of these CIRs, we fit the strahl and halo energy spectra at ∼0.15–1.5 keV to a Kappa function with a Kappa index κ and kinetic temperature T eff. We find that the ∼0.15–1.5 keV strahl electrons behave similarly in both slow and fast wind: the strahl number density n s positively correlates with the solar wind electron temperature T e and interplanetary magnetic field magnitude ∣B∣, while the strahl pitch angle width Θ s decreases with the solar wind speed V sw. These suggest that the strahl electrons are generated by a similar/same process at the Sun in both slow and fast wind that produces these correlations, and the scattering efficiency of strahl in the interplanetary medium (IPM) decreases with V sw. The ∼0.15–1.5 keV halo electrons also behave similarly in both slow and fast wind: the halo parameter positively correlates with the corresponding strahl parameter, and the halo number density n h positively correlates only with T e . These indicate that the halo formation process in the IPM retains most of the strahl properties, but it erases the relationship between n s and ∣B∣. In addition, κ in compressed wind distributes similarly to that in uncompressed wind, for both the strahl and halo. It shows that CIRs at 1 au are not a significant/effective acceleration source for the strahl and halo.

Interplanetary Shock-driven Magnetopause Compressions in Gorgon Global-MHD Simulations

2021 ◽  
Author(s):  
Ravindra Desai ◽  
Jonathan Eastwood ◽  
Joseph Eggington ◽  
Mervyn Freeman ◽  
Martin Archer ◽  
...  
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Interplanetary Shock ◽  
Interplanetary Shocks ◽  
Pressure Balance ◽  
Interplanetary Coronal Mass Ejections ◽  
Corotating Interaction Regions ◽  
Mhd Simulations ◽  
Interaction Regions ◽  
Space Weather Event

<p>Fast-forward interplanetary interplanetary shocks, as occur at the forefront of interplanetary coronal mass ejections and at corotating interaction regions, can rapidly compress the magnetopause inside the drift paths of electrons and protons, and expose geosynchonous satellites directly to the solar wind.  Here, we use Gorgon Global-MHD simulations to study the response of the magnetopause to different fast-forward interplanetary shocks, with strengths extending from the median shocks observed during solar minimum up to that representing an extreme space weather event. The subsequent magnetopause response can be characterised by three distinct phases; an initial acceleration as inertial forces are overcome, a rapid compression well-represented by a power law, and large-scale damped oscillatory motion of the order of an Earth radius, prior to reaching pressure-balance equilibrium. The subsolar magnetopause is found to oscillate with notable frequencies in the range of 2–13 mHz over several periods of diminishing amplitudes.  These results provide an explanation for similar large-scale magnetopause oscillations observed previously during the extreme events of August 1972 and March 1991 and highlight why static magnetopause models break down during periods of strong solar wind driving.</p>

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