Study of Cosmic-Ray Intensity Variations Associated with Anomalous, Long-Duration High-Speed Solar Wind Streams in 2003

Solar Physics ◽  
2007 ◽  
Vol 241 (1) ◽  
pp. 171-184 ◽  
Author(s):  
Laxmi Tripathi ◽  
Anil Kumar Tiwari ◽  
S. P. Agrawal
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Long Duration ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

scholarly journals Cosmic Ray Signatures of Different Types of Solar Wind Streams

1990 ◽  
Vol 142 ◽  
pp. 259-260
Author(s):  
P.K. Shrivastava ◽  
S.P. Agrawal
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Solar Wind Speed ◽  
Coronal Holes ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Wind Speeds ◽  
Different Types ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

The earlier concept of average solar wind speed has changed with time. Besides quiet periods of low/average solar wind speeds, two different kinds of solar sources (solar flares and coronal holes) have been identified to produce high speed solar wind streams. In an earlier investigation, it was reported that the high speed streams associated to these sources produce distinctly different effects on the cosmic ray intensity (Venkatesan, et. al., 1982).

North-south cosmic ray asymmetry and high speed solar wind

1997 ◽  
Vol 19 (6) ◽  
pp. 929-932 ◽  
Author(s):  
A.K. Svirzhevskaya ◽  
G.A. Bazilevskaya ◽  
N.S. Svirzhevsky ◽  
M.B. Krainev
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Cosmic Ray ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

scholarly journals Cross-correlation and cross-wavelet analyses of the solar wind IMF <i>B</i><sub><i>z</i></sub> and auroral electrojet index AE coupling during HILDCAAs

2018 ◽  
Vol 36 (1) ◽  
pp. 205-211 ◽  
Author(s):  
Adriane Marques de Souza ◽  
Ezequiel Echer ◽  
Mauricio José Alves Bolzan ◽  
Rajkumar Hajra
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Cross Correlation ◽  
Auroral Electrojet ◽  
Long Duration ◽  
Ae Index ◽  
Speed Solar Wind ◽  
Wavelet Analyses ◽  
Cross Wavelet ◽  
High Speed Solar Wind

Abstract. Solar-wind–geomagnetic activity coupling during high-intensity long-duration continuous AE (auroral electrojet) activities (HILDCAAs) is investigated in this work. The 1 min AE index and the interplanetary magnetic field (IMF) Bz component in the geocentric solar magnetospheric (GSM) coordinate system were used in this study. We have considered HILDCAA events occurring between 1995 and 2011. Cross-wavelet and cross-correlation analyses results show that the coupling between the solar wind and the magnetosphere during HILDCAAs occurs mainly in the period ≤ 8 h. These periods are similar to the periods observed in the interplanetary Alfvén waves embedded in the high-speed solar wind streams (HSSs). This result is consistent with the fact that most of the HILDCAA events under present study are related to HSSs. Furthermore, the classical correlation analysis indicates that the correlation between IMF Bz and AE may be classified as moderate (0.4–0.7) and that more than 80 % of the HILDCAAs exhibit a lag of 20–30 min between IMF Bz and AE. This result corroborates with Tsurutani et al. (1990) where the lag was found to be close to 20–25 min. These results enable us to conclude that the main mechanism for solar-wind–magnetosphere coupling during HILDCAAs is the magnetic reconnection between the fluctuating, negative component of IMF Bz and Earth's magnetopause fields at periods lower than 8 h and with a lag of about 20–30 min. Keywords. Magnetospheric physics (solar-wind–magnetosphere interactions)

scholarly journals Cosmic Ray Nucleonic Intensity in Low-Amplitude Days During the Passage of High-Speed Solar Wind Streams

2008 ◽  
Vol 45 (2) ◽  
pp. 61-66
Author(s):  
Rekha Agarwal ◽  
Rajesh Mishra ◽  
Sharad Tiwari
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Wave Train ◽  
Cosmic Ray ◽  
Geomagnetic Disturbances ◽  
Start Time ◽  
Plasma Parameters ◽  
Speed Solar Wind ◽  
Low Amplitude ◽  
High Speed Solar Wind

Cosmic Ray Nucleonic Intensity in Low-Amplitude Days During the Passage of High-Speed Solar Wind StreamsOne of the most striking features of solar wind is its organization into high- and low- speed streams. It is now well established that the passage over the Earth of high-speed solar wind streams leads to geomagnetic disturbances. The high-speed plasma streams are thus a key element in the complex chain of events that link geomagnetic activity to the solar activity and are therefore of great interest to the solar terrestrial physics. Two types of high-speed solar wind streams - coronal-hole-associated (or corotating) and flare-generated - were studied based on magnetic field and solar wind plasma parameters. In the work, the dependence was obtained for cosmic ray (CR) depressions due to high-speed solar wind streams during low-amplitude days. The CR nucleonic intensity data were subjected to the superposed epoch analysis with respect to the start time of high-speed solar wind streams. It was found that streams of both types produce significant deviations in the CR intensity during low-amplitude anisotropic wave train events. At the onset of such streams the CR intensity reaches its minimum during low-amplitude events and then increases statistically.

A periodical analysis of the cosmic-ray diffusion coefficient and the high-speed solar-wind streams

1988 ◽  
Vol 43 (2) ◽  
pp. 165-179
Author(s):  
J. Xanthakis ◽  
H. Mavromichalaki ◽  
B. Petropoulos ◽  
E. Marmatsouri ◽  
A. Vassilaki
Keyword(s):  
Solar Wind ◽  
Diffusion Coefficient ◽  
High Speed ◽  
Cosmic Ray ◽  
Speed Solar Wind ◽  
Ray Diffusion ◽  
High Speed Solar Wind

High-speed solar-wind streams and galactic cosmic-ray modulation

1979 ◽  
Vol 2 (4) ◽  
pp. 421-438 ◽  
Author(s):  
N. Iucci ◽  
M. Parisi ◽  
M. Storini ◽  
G. Villoresi
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Cosmic Ray ◽  
Cosmic Ray Modulation ◽  
Speed Solar Wind ◽  
Galactic Cosmic Ray ◽  
High Speed Solar Wind
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