scholarly journals Motion of the dusk flank boundary layer caused by solar wind pressure changes and the Kelvin-Helmholtz instability: 10–11 January 1997

2003 ◽  
Vol 108 (A12) ◽  
Author(s):  
D. H. Fairfield
Keyword(s):  
Boundary Layer ◽  
Solar Wind ◽  
Wind Pressure ◽  
Helmholtz Instability ◽  
Solar Wind Pressure ◽  
Pressure Changes

scholarly journals An unusual giant spiral arc in the polar cap region during the northward phase of a Coronal Mass Ejection

2007 ◽  
Vol 25 (2) ◽  
pp. 507-517 ◽  
Author(s):  
L. Rosenqvist ◽  
A. Kullen ◽  
S. Buchert
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Spiral Structure ◽  
Wind Pressure ◽  
Polar Cap ◽  
Sheath Region ◽  
Interplanetary Coronal Mass Ejection ◽  
Solar Wind Pressure ◽  
Pressure Changes ◽  
Mass Ejection

Abstract. The shock arrival of an Interplanetary Coronal Mass Ejection (ICME) at ~09:50 UT on 22 November 1997 resulted in the development of an intense (Dst<−100 nT) geomagnetic storm at Earth. In the early, quiet phase of the storm, in the sheath region of the ICME, an unusual large spiral structure (diameter of ~1000 km) was observed at very high latitudes by the Polar UVI instrument. The evolution of this structure started as a polewardly displaced auroral bulge which further developed into the spiral structure spreading across a large part of the polar cap. This study attempts to examine the cause of the chain of events that resulted in the giant auroral spiral. During this period the interplanetary magnetic field (IMF) was dominantly northward (Bz>25 nT) with a strong duskward component (By>15 nT) resulting in a highly twisted tail plasma sheet. Geotail was located at the equatorial dawnside magnetotail flank and observed accelerated plasma flows exceeding the solar wind bulk velocity by almost 60%. These flows are observed on the magnetosheath side of the magnetopause and the acceleration mechanism is proposed to be typical for strongly northward IMF. Identified candidates to the cause of the spiral structure include a By induced twisted magnetotail configuration, the development of magnetopause surface waves due to the enhanced pressure related to the accelerated magnetosheath flows aswell as the formation of additional magnetopause deformations due to external solar wind pressure changes. The uniqeness of the event indicate that most probably a combination of the above effects resulted in a very extreme tail topology. However, the data coverage is insufficient to fully investigate the physical mechanism behind the observations.

scholarly journals Solar wind and substorm excitation of the wavy current sheet

2009 ◽  
Vol 27 (6) ◽  
pp. 2457-2474 ◽  
Author(s):  
C. Forsyth ◽  
M. Lester ◽  
R. C. Fear ◽  
E. Lucek ◽  
I. Dandouras ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Current Sheet ◽  
Pressure Pulse ◽  
Wind Pressure ◽  
Expansion Velocity ◽  
Solar Wind Pressure ◽  
Wave Models ◽  
Best Fit ◽  
The Magnetic Field

Abstract. Following a solar wind pressure pulse on 3 August 2001, GOES 8, GOES 10, Cluster and Polar observed dipolarizations of the magnetic field, accompanied by an eastward expansion of the aurora observed by IMAGE, indicating the occurrence of two substorms. Prior to the first substorm, the motion of the plasma sheet with respect to Cluster was in the ZGSM direction. Observations following the substorms show the occurrence of current sheet waves moving predominantly in the −YGSM direction. Following the second substorm, the current sheet waves caused multiple current sheet crossings of the Cluster spacecraft, previously studied by Zhang et al. (2002). We further this study to show that the velocity of the current sheet waves was similar to the expansion velocity of the substorm aurora and the expansion of the dipolarization regions in the magnetotail. Furthermore, we compare these results with the current sheet wave models of Golovchanskaya and Maltsev (2005) and Erkaev et al. (2008). We find that the Erkaev et al. (2008) model gives the best fit to the observations.

scholarly journals Induced and Permanent Magnetism on the Moon: Structural and Evolutionary Implications

1971 ◽  
Vol 2 ◽  
pp. 173-188
Author(s):  
C. P. Sonett ◽  
P. Dyal ◽  
D. S. Colburn ◽  
B. F. Smith ◽  
G. Schubert ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Dynamic Pressure ◽  
Wind Pressure ◽  
Dark Side ◽  
The Moon ◽  
Permanent Magnetic Field ◽  
Crustal Layer ◽  
Induced Field ◽  
Solar Wind Pressure

AbstractIt is shown that the Moon possesses an extraordinary response to induction from the solar wind due to a combination of a high interior electrical conductivity together with a relatively resistive crustal layer into which the solar wind dynamic pressure forces back the induced field. The dark side response, devoid of solar wind pressure, is approximately that expected for the vacuum case. These data permit an assessment of the interior conductivity and an estimate of the thermal gradient in the crustal region. The discovery of a large permanent magnetic field at the Apollo 12 site corresponds approximately to the paleomagnetic residues discovered in both Apollo 11 and 12 rock samples The implications regarding an early lunar magnetic field are discussed and it is shown that among the various conjectures regarding the early field the most prominent are either an interior dynamo or an early approach to the Earth though no extant model is free of difficulties.

The role of solar wind pressure jumps in the initiation and control processes of magnetospheric substorms

2011 ◽  
Vol 51 (7) ◽  
pp. 979-993 ◽  
Author(s):  
V. A. Parkhomov ◽  
N. L. Borodkova ◽  
A. V. Dmitriev ◽  
P. M. Klimov ◽  
R. A. Rakhmatulin
Keyword(s):  
Solar Wind ◽  
Wind Pressure ◽  
Magnetospheric Substorms ◽  
Control Processes ◽  
Solar Wind Pressure ◽  
And Control

scholarly journals Dayside magnetospheric and ionospheric responses to solar wind pressure increase: Multispacecraft and ground observations

2016 ◽  
Vol 121 (11) ◽  
pp. 10,813-10,830 ◽  
Author(s):  
A. M. Tian ◽  
X. C. Shen ◽  
Q. Q. Shi ◽  
B. B. Tang ◽  
M. Nowada ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wind Pressure ◽  
Pressure Increase ◽  
Solar Wind Pressure
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