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

scholarly journals Changes of dayside auroral distribution caused by a solar wind pressure pulse and associated interplanetary magnetic field disturbances

2007 ◽  
Vol 25 (4) ◽  
pp. 929-940 ◽  
Author(s):  
A. Kozlovsky ◽  
M. Meurant ◽  
T. Turunen
Keyword(s):  
Solar Wind ◽  
Auroral Oval ◽  
Wind Pressure ◽  
Pressure Increase ◽  
Polar Cap ◽  
Related System ◽  
Obvious Effect ◽  
Image Satellite ◽  
Solar Wind Pressure ◽  
The Imf

Abstract. Global auroral images from the IMAGE satellite were used to study statistically changes of the dayside aurora spatial distribution after an abrupt solar wind pressure increase, or so-called "Sudden Impulse" (SI). Contributions from IMF changes associated with a SI were also investigated. The effects of the IMF and pressure variations were separated using a multi-factor correlation analysis. The first prominent effect due to pressure increase is the auroral intensification equatorward of the middle dayside oval within 6 min after a SI occurred. This is consistent with the midday sub-auroral patches. The second effect due to pressure increase is the auroral intensification at high latitudes in the vicinity of the polar cap boundary. For the first 6 min the auroral intensification is most prominent in the postnoon sector. Later on (6–20 min) the intensification occurs in the prenoon sector. The most obvious effect of IMF changes is the "IMF By" effect, an intensification (fading) of the most poleward auroral forms when IMF By becomes negative (positive). This effect occurs 6–20 min after changes in the interplanetary medium. Such an effect is consistent with the IMF By-related system of field-aligned currents. No significant motion of the dayside auroral oval was observed associated with IMF Bz variations. This can be explained by a response time to IMF Bz changes larger than 20 min.

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 Ionospheric signatures of plasma injections in the cusp triggered by solar wind pressure pulses

2005 ◽  
Vol 110 (A8) ◽  
Author(s):  
Jean-Claude Cerisier ◽  
Aurélie Marchaudon ◽  
Jean-Michel Bosqued ◽  
Kathryn McWilliams ◽  
Harald U. Frey ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wind Pressure ◽  
Pressure Pulses ◽  
Solar Wind Pressure
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