scholarly journals Buildup of the ring current during periodic loading-unloading cycles in the magnetotail driven by steady southward interplanetary magnetic field

2007 ◽  
Vol 112 (A9) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. Taktakishvili ◽  
M. M. Kuznetsova ◽  
M. Hesse ◽  
M.-C. Fok ◽  
L. Rastätter ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ring Current ◽  
Periodic Loading

scholarly journals Simulated ring current response during periods of dawn-dusk oriented interplanetary magnetic field (By)

2013 ◽  
Vol 118 (5) ◽  
pp. 2228-2243 ◽  
Author(s):  
Elizabeth J. Mitchell ◽  
Mei-Ching H. Fok ◽  
Ramon E. Lopez ◽  
John G. Lyon
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ring Current ◽  
Current Response

scholarly journals Azimuthally asymmetric ring current as a function of <i>D<sub>st</sub></i> and solar wind conditions

2004 ◽  
Vol 22 (8) ◽  
pp. 2989-2996 ◽  
Author(s):  
Y. P. Maltsev ◽  
A. A. Ostapenko
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Spatial Distribution ◽  
Interplanetary Magnetic Field ◽  
Ring Current ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Magnetic Data ◽  
Under Five ◽  
Solar Wind Parameters

Abstract. Based on magnetic data, spatial distribution of the westward ring current flowing at |z|<3 RE has been found under five levels of Dst, five levels of the interplanetary magnetic field (IMF) z component, and five levels of the solar wind dynamic pressure Psw. The maximum of the current is located near midnight at distances 5 to 7 RE. The magnitude of the nightside and dayside parts of the westward current at distances from 4 to 9 RE can be approximated as Inight=1.75-0.041 Dst, Inoon=0.22-0.013 Dst, where the current is in MA. The relation of the nightside current to the solar wind parameters can be expressed as Inight=1.45-0.20 Bs IMF + 0.32 Psw, where BsIMF is the IMF southward component. The dayside ring current poorly correlates with the solar wind parameters.

scholarly journals Characteristics of the electrojet during intense magnetic disturbances

2018 ◽  
Vol 36 (5) ◽  
pp. 1361-1391
Author(s):  
Liudmila I. Gromova ◽  
Matthias Förster ◽  
Yakov I. Feldstein ◽  
Patricia Ritter
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ring Current ◽  
Flow Direction ◽  
Field Measurements ◽  
Main Phase ◽  
Champ Satellite ◽  
Electrojet Current ◽  
Magnetic Disturbances ◽  
The Imf

Abstract. Hall current variations in different time sectors during six magnetic storms from the summer seasons in 2003 and 2005 (Ritter, 2018) are examined, namely three storms in the day–night meridional sector and three storms in the dawn–dusk sector. The sequence of the phenomena, their structure and positions, and the strength of the polar (PE) and the auroral (AE) Hall electrojets were investigated using scalar magnetic field measurements obtained from the CHAllenging Minisatellite Payload (CHAMP) satellite in accordance with the study of Ritter et al. (2004a). We analyzed the correlations of the PE and AE as well as the obtained regression relations of the magnetic latitude MLat and the electrojet current intensity I with auroral and ring current activity, the interplanetary magnetic field, and the Newell et al. (2007) coupling function for the state of the solar wind. The following typical characteristics of the electrojets were revealed: The PE appears in the daytime sector at MLat ∼80∘–73∘, with a westward or an eastward direction depending on the interplanetary magnetic field (IMF) By component (By < 0 nT or By > 0 nT). Changes in the current flow direction in the PE can occur repeatedly during the storm, but only due to changes in the IMF By orientation. The PE increases with the intensity of the IMF By component from I∼0.4 A m−1 for By∼0 nT up to I∼1.0 A m−1 for By∼23 nT. The MLat position of the PE does not depend on the direction and intensity of the By component. There is no connection between MLat and I in the PE and the symmetric part of the magnetospheric ring current (index SymH). There is a correlation between I in the PE and the AsyH index, but only a very weak interconnection of this index with the MLat of the PE. Substorms occurring before the storm's main phase are accompanied by the appearance of an eastward electrojet (EE) at MLat ∼64∘ as well as that of a westward electrojet (WE). In the nighttime sector, a WE appears at MLat ∼64∘. During the main phase both electrojets persist. The daytime EE and the nighttime WE shift toward sub-auroral latitudes of MLat ∼56∘ and grow in intensity up to I∼1.5 A m−1. The WE is then located about 6∘ closer to the pole than the EE during evening hours and about 2∘–3∘ closer during daytime hours.

H-Cmes and Ii-Type Radio Bursts Related Intense Geomagnetic Storms in Relation With Interplanetary Magnetic Field and Solar Wind Disturbances

2012 ◽  
Vol 2 (10) ◽  
pp. 1-3 ◽  
Author(s):  
Praveen Kumar Gupta ◽  
◽  
Puspraj Singh Puspraj Singh ◽  
Puspraj Singh Puspraj Singh ◽  
P. K. Chamadia P. K. Chamadia
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Storms ◽  
Radio Bursts ◽  
Solar Wind Disturbances

The polarity pattern of the interplanetary magnetic field during solar rotations 1798-1808

1967 ◽  
Vol 72 (5) ◽  
pp. 1637-1643 ◽  
Author(s):  
Paul J. Coleman ◽  
Leverett Davis ◽  
Edward J. Smith ◽  
Douglas E. Jones
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field
Sign in / Sign up

Export Citation Format

Share Document