The quiet geomagnetic field at geosynchronous orbit and its dependence on solar wind dynamic pressure

1992 ◽  
Vol 97 (A1) ◽  
pp. 25 ◽  
Author(s):  
Clifford L. Rufenach ◽  
Robert L. McPherron ◽  
Justin Schaper
Keyword(s):  
Solar Wind ◽  
Geomagnetic Field ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Geosynchronous Orbit

scholarly journals ULF waves excited by negative/positive solar wind dynamic pressure impulses at geosynchronous orbit

2010 ◽  
Vol 115 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
X. Y. Zhang ◽  
Q.-G. Zong ◽  
Y. F. Wang ◽  
H. Zhang ◽  
L. Xie ◽  
...  
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Geosynchronous Orbit ◽  
Ulf Waves

Direct detection of solar wind dynamic pressure effect on ground geomagnetic field

1993 ◽  
Vol 20 (9) ◽  
pp. 775-778 ◽  
Author(s):  
T. Araki ◽  
K. Funato ◽  
T. Iguchi ◽  
T. Kamei
Keyword(s):  
Solar Wind ◽  
Geomagnetic Field ◽  
Pressure Effect ◽  
Direct Detection ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure

scholarly journals Geosynchronous magnetic field responses to fast solar wind dynamic pressure enhancements: MHD field model

2012 ◽  
Vol 30 (8) ◽  
pp. 1285-1295 ◽  
Author(s):  
T. R. Sun ◽  
C. Wang ◽  
N. L. Borodkova ◽  
G. N. Zastenker
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Field Model ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Geosynchronous Orbit ◽  
Total Field ◽  
Fast Solar Wind ◽  
Dominant Component ◽  
Mhd Simulations

Abstract. We performed global MHD simulations of the geosynchronous magnetic field in response to fast solar wind dynamic pressure (Pd) enhancements. Taking three Pd enhancement events in 2000 as examples, we found that the main features of the total field B and the dominant component Bz can be efficiently predicted by the MHD model. The predicted B and Bz varies with local time, with the highest level near noon and a slightly lower level around mid-night. However, it is more challenging to accurately predict the responses of the smaller component at the geosynchronous orbit (i.e., Bx and By). In contrast, the limitations of T01 model in predicting responses to fast Pd enhancements are presented.

Solar wind dynamic pressure enhancements and polar auroras

1998 ◽  
Vol 22 (9) ◽  
pp. 1305-1308 ◽  
Author(s):  
Y Zhang ◽  
D.J McEwen ◽  
I Oznovich
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure
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