scholarly journals A Numerical Study of the Effects of Corotating Interaction Regions on Cosmic-Ray Transport

2020 ◽  
Vol 899 (2) ◽  
pp. 90 ◽  
Author(s):  
Xi Luo ◽  
Ming Zhang ◽  
Xueshang Feng ◽  
Marius S Potgieter ◽  
Fang Shen ◽  
...  
Keyword(s):  
Numerical Study ◽  
Cosmic Ray ◽  
Corotating Interaction Regions ◽  
Interaction Regions

Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions

2017 ◽  
Vol 837 (1) ◽  
pp. 37 ◽  
Author(s):  
Andreas Kopp ◽  
Tobias Wiengarten ◽  
Horst Fichtner ◽  
Frederic Effenberger ◽  
Patrick Kühl ◽  
...  
Keyword(s):  
Particle Transport ◽  
Cosmic Ray ◽  
Corotating Interaction Regions ◽  
Magnetic Structures ◽  
Interaction Regions

scholarly journals On Cosmic Rays, IP Structures and Geospace Consequences During WHI

2009 ◽  
Vol 5 (H15) ◽  
pp. 488-490
Author(s):  
A. Dal Lago ◽  
F. L. Guarnieri ◽  
M. R. da Silva ◽  
W. D. Gonzalez ◽  
C. R. Braga ◽  
...  
Keyword(s):  
High Speed ◽  
Interplanetary Space ◽  
Cosmic Ray ◽  
Corotating Interaction Regions ◽  
Near Earth Space ◽  
Long Duration ◽  
Minimum Solar Activity ◽  
Interaction Regions ◽  
Muon Detection ◽  
Whole Heliosphere Interval

AbstractThis work presents some observations during the period of the Whole Heliosphere Interval (WHI) of the effects of interplanetary (IP) structures on the near-Earth space using three sets of observations: magnetic field and plasma from the Advanced Composition Explorer (ACE) satellite, ground-based cosmic ray data from the Global Muon Detection Network (GMDN) and geomagnetic indices (Disturbance storm-time, Dst, and auroral electrojet index, AE). Since WHI was near minimum solar activity, high speed streams and corotating interaction regions (CIRs) were the dominant structures observed in the interplanetary space surrounding Earth. Very pronounced geomagnetic effects are shown to be correlated to CIRs, especially because they can cause the so-called High-Intensity Long-Duration Continuous AE Activity (HILDCAAs) - Tsurutani and Gonzalez (1987). At least a few high speed streams can be identified during the period of WHI. The focus here is to characterize these IP structures and their geospace consequences.

scholarly journals Cosmic ray modulation by corotating interaction regions

2008 ◽  
Vol 4 (S257) ◽  
pp. 425-427 ◽  
Author(s):  
Jaša Čalogović ◽  
Bojan Vršnak ◽  
Manuela Temmer ◽  
Astrid M. Veronig
Keyword(s):  
Solar Wind ◽  
Time Lag ◽  
Cosmic Ray ◽  
Central Meridian ◽  
Corotating Interaction Regions ◽  
Cosmic Ray Modulation ◽  
Cross Correlation Analysis ◽  
Interaction Regions ◽  
The Relationship

AbstractWe analyzed the relationship between the ground-based modulation of cosmic rays (CR) and corotating interaction regions (CIRs). Daily averaged data from 8 different neutron monitor (NM) stations were used, covering rigidities from Rc = 0 − 12.91 GeV. The in situ solar wind data were taken from the Advanced Composition Explorer (ACE) database, whereas the coronal hole (CH) areas were derived from the Solar X-Ray Imager onboard GOES-12. For the analysis we have chosen a period in the declining phase of solar cycle 23, covering the period 25 January–5 May 2005. During the CIR periods CR decreased typically from 0.5% to 2%. A cross-correlation analysis showed a distinct anti-correlation between the magnetic field and CR, with the correlation coefficient (r) ranging from −0.31 to −0.38 (mean: −0.36) and with the CR time delay of 2 to 3 days. Similar anti-correlations were found for the solar wind density and velocity characterized by the CR time lag of 4 and 1 day, respectively. The relationship was also established between the CR modulation and the area of the CIR-related CH with the CR time lag of 5 days after the central-meridian passage of CH.

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

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.

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