Injection and Acceleration Processes in Corotating Interaction Regions: Theoretical Concepts

1999 ◽  
pp. 105-114
Author(s):  
Manfred Scholer
Keyword(s):  
Corotating Interaction Regions ◽  
Theoretical Concepts ◽  
Interaction Regions

scholarly journals Corotating Interaction Regions as Seen by the STEREO Heliospheric Imagers 2007 – 2010

Solar Physics ◽  
2015 ◽  
Vol 290 (8) ◽  
pp. 2291-2309 ◽  
Author(s):  
T. M. Conlon ◽  
S. E. Milan ◽  
J. A. Davies ◽  
A. O. Williams
Keyword(s):  
Corotating Interaction Regions ◽  
Interaction Regions

Study of Corotating Interaction Regions in the Ascending Phase of the Solar Cycle: Multi-spacecraft Observations

Solar Physics ◽  
2013 ◽  
Vol 285 (1-2) ◽  
pp. 201-216 ◽  
Author(s):  
J. A. Gonzalez-Esparza ◽  
E. Romero-Hernandez ◽  
P. Riley
Keyword(s):  
Solar Cycle ◽  
Corotating Interaction Regions ◽  
Interaction Regions

Changes in cosmic ray propagation induced by corotating interaction regions

1981 ◽  
Vol 1 (3) ◽  
pp. 155-158
Author(s):  
R. Gall ◽  
B.T. Thomas ◽  
G. Vidargas
Keyword(s):  
Cosmic Ray ◽  
Corotating Interaction Regions ◽  
Interaction Regions

scholarly journals On the origin of variable structures in the winds of hot luminous stars

2013 ◽  
Vol 440 (1) ◽  
pp. 2-9 ◽  
Author(s):  
Yannick J. L. Michaux ◽  
Anthony F. J. Moffat ◽  
André-Nicolas Chené ◽  
Nicole St-Louis
Keyword(s):  
Magnetic Field ◽  
Empirical Evidence ◽  
Temporal Variability ◽  
Large Scale ◽  
Small Scale ◽  
Ionization Zone ◽  
Corotating Interaction Regions ◽  
Wind Variability ◽  
Global Magnetic Field ◽  
Interaction Regions

Abstract Examination of the temporal variability properties of several strong optical recombination lines in a large sample of Galactic Wolf–Rayet (WR) stars reveals possible trends, especially in the more homogeneous WC than the diverse WN subtypes, of increasing wind variability with cooler subtypes. This could imply that a serious contender for the driver of the variations is stochastic, magnetic subsurface convection associated with the 170 kK partial-ionization zone of iron, which should occupy a deeper and larger zone of greater mass in cooler WR subtypes. This empirical evidence suggests that the heretofore proposed ubiquitous driver of wind variability, radiative instabilities, may not be the only mechanism playing a role in the stochastic multiple small-scaled structures seen in the winds of hot luminous stars. In addition to small-scale stochastic behaviour, subsurface convection guided by a global magnetic field with localized emerging loops may also be at the origin of the large-scale corotating interaction regions as seen frequently in O stars and occasionally in the winds of their descendant WR stars.

Muon and neutron observations in connection with the corotating interaction regions

2007 ◽  
Vol 40 (3) ◽  
pp. 348-352 ◽  
Author(s):  
M.R. Da Silva ◽  
A. Dal Lago ◽  
E. Echer ◽  
A. de Lucas ◽  
W.D. Gonzalez ◽  
...  
Keyword(s):  
Corotating Interaction Regions ◽  
Interaction Regions

Stream interfaces and energetic ions in corotating interaction regions: Ulysses test of Pioneer results

1996 ◽  
Author(s):  
Devrie S. Intriligator ◽  
George L. Siscoe ◽  
Gerd Wibberenz ◽  
Horst Kunow ◽  
John T. Gosling
Keyword(s):  
Corotating Interaction Regions ◽  
Energetic Ions ◽  
Interaction Regions
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