scholarly journals Substorm activity on January 11, 1994: Geotail observations in the distant tail during the leading phase of a corotating interaction region

1998 ◽  
Vol 103 (A8) ◽  
pp. 17671-17689 ◽  
Author(s):  
B. Wilken ◽  
Q.-G. Zong ◽  
T. Doke ◽  
T. Mukai ◽  
T. Yamamoto ◽  
...  
Keyword(s):  
Interaction Region ◽  
Corotating Interaction Region ◽  
Substorm Activity

scholarly journals Ionospheric storms on Mars: Impact of the corotating interaction region

2009 ◽  
Vol 36 (1) ◽  
Author(s):  
E. Dubinin ◽  
M. Fraenz ◽  
J. Woch ◽  
F. Duru ◽  
D. Gurnett ◽  
...  
Keyword(s):  
Interaction Region ◽  
Corotating Interaction Region

scholarly journals Ionospheric response to the corotating interaction region-driven geomagnetic storm of October 2002

2009 ◽  
Vol 114 (A12) ◽  
pp. n/a-n/a ◽  
Author(s):  
D. Pokhotelov ◽  
C. N. Mitchell ◽  
P. T. Jayachandran ◽  
J. W. MacDougall ◽  
M. H. Denton
Keyword(s):  
Geomagnetic Storm ◽  
Interaction Region ◽  
Corotating Interaction Region ◽  
Ionospheric Response

scholarly journals Response of the total electron content at Brazilian low latitudes to corotating interaction region and high-speed streams during solar minimum 2008

2018 ◽  
Vol 70 (1) ◽  
Author(s):  
Claudia M. N. Candido ◽  
Inez S. Batista ◽  
Virginia Klausner ◽  
Patricia M. de Siqueira Negreti ◽  
Fabio Becker-Guedes ◽  
...  
Keyword(s):  
Total Electron Content ◽  
Solar Minimum ◽  
High Speed ◽  
Interaction Region ◽  
Electron Content ◽  
Corotating Interaction Region ◽  
Total Electron ◽  
Low Latitudes

Perpendicular Transport of Low-Energy Corotating Interaction Region–associated Nuclei

1997 ◽  
Vol 490 (1) ◽  
pp. L115-L118 ◽  
Author(s):  
J. R. Dwyer ◽  
G. M. Mason ◽  
J. E. Mazur ◽  
J. R. Jokipii ◽  
T. T. von Rosenvinge ◽  
...  
Keyword(s):  
Interaction Region ◽  
Low Energy ◽  
Corotating Interaction Region

scholarly journals Acceleration of Energetic Ions in Corotating Interaction Region near 1.5 au: Evidence from MAVEN

2019 ◽  
Vol 880 (1) ◽  
pp. L3 ◽  
Author(s):  
Smitha V. Thampi ◽  
C. Krishnaprasad ◽  
P. R. Shreedevi ◽  
Tarun Kumar Pant ◽  
Anil Bhardwaj
Keyword(s):  
Interaction Region ◽  
Corotating Interaction Region ◽  
Energetic Ions

scholarly journals Modelling three-dimensional transport of solar energetic protons in a corotating interaction region generated with EUHFORIA

2019 ◽  
Vol 622 ◽  
pp. A28 ◽  
Author(s):  
N. Wijsen ◽  
A. Aran ◽  
J. Pomoell ◽  
S. Poedts
Keyword(s):  
Solar Wind ◽  
Interplanetary Space ◽  
High Energy ◽  
Interaction Region ◽  
Corotating Interaction Region ◽  
Fast Solar Wind ◽  
Transport Code ◽  
Field Diffusion ◽  
Forward Shock ◽  
The Cross

Aims. We introduce a new solar energetic particle (SEP) transport code that aims at studying the effects of different background solar wind configurations on SEP events. In this work, we focus on the influence of varying solar wind velocities on the adiabatic energy changes of SEPs and study how a non-Parker background solar wind can trap particles temporarily at small heliocentric radial distances (≲1.5 AU) thereby influencing the cross-field diffusion of SEPs in the interplanetary space. Methods. Our particle transport code computes particle distributions in the heliosphere by solving the focused transport equation (FTE) in a stochastic manner. Particles are propagated in a solar wind generated by the newly developed data-driven heliospheric model, EUHFORIA. In this work, we solve the FTE, including all solar wind effects, cross-field diffusion, and magnetic-field gradient and curvature drifts. As initial conditions, we assume a delta injection of 4 MeV protons, spread uniformly over a selected region at the inner boundary of the model. To verify the model, we first propagate particles in nominal undisturbed fast and slow solar winds. Thereafter, we simulate and analyse the propagation of particles in a solar wind containing a corotating interaction region (CIR). We study the particle intensities and anisotropies measured by a fleet of virtual observers located at different positions in the heliosphere, as well as the global distribution of particles in interplanetary space. Results. The differential intensity-time profiles obtained in the simulations using the nominal Parker solar wind solutions illustrate the considerable adiabatic deceleration undergone by SEPs, especially when propagating in a fast solar wind. In the case of the solar wind containing a CIR, we observe that particles adiabatically accelerate when propagating in the compression waves bounding the CIR at small radial distances. In addition, for r ≳ 1.5 AU, there are particles accelerated by the reverse shock as indicated by, for example, the anisotropies and pitch-angle distributions of the particles. Moreover, a decrease in high-energy particles at the stream interface (SI) inside the CIR is observed. The compression/shock waves and the magnetic configuration near the SI may also act as a magnetic mirror, producing long-lasting high intensities at small radial distances. We also illustrate how the efficiency of the cross-field diffusion in spreading particles in the heliosphere is enhanced due to compressed magnetic fields. Finally, the inclusion of cross-field diffusion enables some particles to cross both the forward compression wave at small radial distances and the forward shock at larger radial distances. This results in the formation of an accelerated particle population centred on the forward shock, despite the lack of magnetic connection between the particle injection region and this shock wave. Particles injected in the fast solar wind stream cannot reach the forward shock since the SI acts as a diffusion barrier.

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