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 Development of substorm bulges during different solar wind structures

2009 ◽  
Vol 27 (5) ◽  
pp. 1951-1960 ◽  
Author(s):  
I. V. Despirak ◽  
A. A. Lubchich ◽  
A. G. Yahnin ◽  
B. V. Kozelov ◽  
H. K. Biernat
Keyword(s):  
Solar Wind ◽  
Ultra Violet ◽  
Magnetic Clouds ◽  
Corotating Interaction Regions ◽  
Longitudinal Size ◽  
Solar Wind Flow ◽  
Wind Spacecraft ◽  
The Difference ◽  
Interaction Regions ◽  
Using Data

Abstract. Using data from WIND spacecraft, we investigated the difference in substorm bulge development during different types of solar wind flow: solar wind recurrent streams (RS), corotating interaction regions (CIR), magnetic clouds (MC), and the region of interaction of magnetic clouds with undisturbed solar wind (Sheath). The RS/CIR and MC/Sheath structures were examined for the periods December 1996–July 1997; January 2000–December 2000; October 2001. All available auroral substorms observed by the Ultra Violet Imager onboard the Polar spacecraft during these periods were studied. It is shown that the largest latitudinal and longitudinal sizes of the auroral bulge expansions are during CIR and Sheath intervals. We found a difference in auroral bulge parameters for MC- and RS-associated substorms. In contrast to substorms associated with RS, the latitudinal size of the auroral bulge during MC is smaller, but longitudinal size is larger. As consequence, the ratio between longitudinal and latitudinal sizes for MC-associated substorms is also larger. We suggest that the latter feature is explained by different configuration of the near-Earth magnetotail during RS and MC.

Solar wind flow past Venus and its implications for the occurrence of the Kelvin–Helmholtz instability

2007 ◽  
Vol 55 (12) ◽  
pp. 1793-1803 ◽  
Author(s):  
H.K. Biernat ◽  
N.V. Erkaev ◽  
U.V. Amerstorfer ◽  
T. Penz ◽  
H.I.M. Lichtenegger
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Helmholtz Instability ◽  
Flow Past ◽  
Solar Wind Flow

Effects on the Jovian magnetosheath arising from solar wind flow around nonaxisymmetric bodies

1996 ◽  
Vol 101 (A5) ◽  
pp. 10665-10672 ◽  
Author(s):  
N. V. Erkaev ◽  
C. J. Farrugia ◽  
H. K. Biernat
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Solar Wind Flow

Estimation of the entropy of the solar wind flow

2000 ◽  
Vol 62 (5) ◽  
pp. 6496-6504 ◽  
Author(s):  
Wiesław M. Macek ◽  
Stefano Redaelli
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Solar Wind Flow

Genesis On-board Determination of the Solar Wind Flow Regime

2003 ◽  
pp. 153-171 ◽  
Author(s):  
M. Neugebauer ◽  
J. T. Steinberg ◽  
R. L. Tokar ◽  
B. L. Barraclough ◽  
E. E. Dors ◽  
...  
Keyword(s):  
Solar Wind ◽  
Flow Regime ◽  
Wind Flow ◽  
Solar Wind Flow

Strong influence of lunar crustal fields on the solar wind flow

2011 ◽  
Vol 38 (3) ◽  
pp. n/a-n/a ◽  
Author(s):  
Charles Lue ◽  
Yoshifumi Futaana ◽  
Stas Barabash ◽  
Martin Wieser ◽  
Mats Holmström ◽  
...  
Keyword(s):  
Solar Wind ◽  
Strong Influence ◽  
Wind Flow ◽  
Solar Wind Flow

Solar-wind flow behind the Moon

1968 ◽  
Vol 73 (13) ◽  
pp. 4281-4289 ◽  
Author(s):  
R. A. Wolf
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
The Moon ◽  
Solar Wind Flow
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