Configurations of Earth’s magnetosphere in response to variations in z component Solar-wind flow during the southward IMF

2020 ◽  
Vol 96 (1) ◽  
pp. 015007
Author(s):  
Lingjie Li
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Solar Wind Flow

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

scholarly journals Space Weather, SuperDARN and the Tasmanian Tiger

1997 ◽  
Vol 50 (4) ◽  
pp. 773 ◽  
Author(s):  
Raymond A. Greenwald
Keyword(s):  
Solar Wind ◽  
Electric Fields ◽  
Space Weather ◽  
Interplanetary Space ◽  
Rapid Evolution ◽  
Upper Atmosphere ◽  
Global Network ◽  
Pressure Gradients ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

The plasma environment extending from the solar surface through interplanetary space to the outermost reaches of the Earth’s atmosphere and magnetic field is dynamic, often disturbed, and capable of harming humans and damaging manmade systems. Disturbances in this environment have been identified as space weather disturbances. At the present time there is growing interest in monitoring and predicting space weather disturbances. In this paper we present some of the difficulties involved in achieving this goal by comparing the processes that drive tropospheric-weather systems with those that drive space-weather systems in the upper atmosphere and ionosphere. The former are driven by pressure gradients which result from processes that heat and cool the atmosphere. The latter are driven by electric fields that result from interactions between the streams of ionised gases emerging from the Sun (solar wind) and the Earth’s magnetosphere. Although the dimensions of the Earth’s magnetosphere are vastly greater than those of tropospheric weather systems, the global space-weather response to changes in the solar wind is much more rapid than the response of tropospheric-weather systems to changing conditions. We shall demonstrate the rapid evolution of space-weather systems in the upper atmosphere through measurements with a global network of radars known as SuperDARN. We shall also describe how the SuperDARN network is evolving, including a newly funded Australian component known as the Tasman International Geospace Environmental Radar (TIGER).

A comparison of predictions of an MHD model solar wind flow past the magnetopause with AMPTE/IRM observations on 24 October, 1985

1998 ◽  
Vol 22 (1) ◽  
pp. 67-72 ◽  
Author(s):  
C.J. Farrugia ◽  
H.K. Biernat ◽  
N.V. Erkaev ◽  
L.M. Kistler
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Flow Past ◽  
Solar Wind Flow ◽  
Mhd Model

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
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