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The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm

Urheber*innen
/persons/resource/dipti

Rout,  D
2.3 Geomagnetism, 2.0 Geophysics, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;

Patra,  S.
External Organizations;

Kumar,  S.
External Organizations;

Chakrabarty,  D.
External Organizations;

Reeves,  G. D.
External Organizations;

Stolle,  C.
External Organizations;

Pandey,  K.
External Organizations;

Chakraborty,  S.
External Organizations;

Spencer,  E. A.
External Organizations;

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5025122.pdf
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Zitation

Rout, D., Patra, S., Kumar, S., Chakrabarty, D., Reeves, G. D., Stolle, C., Pandey, K., Chakraborty, S., Spencer, E. A. (2023): The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm. - Space Weather, 21, 10, e2023SW003489.
https://doi.org/10.1029/2023SW003489


Zitierlink: https://gfzpublic.gfz-potsdam.de/pubman/item/item_5025122
Zusammenfassung
The total energy transfer from the solar wind to the magnetosphere is governed by the reconnection rate at the magnetosphere edges as the Z-component of interplanetary magnetic field (IMF Bz) turns southward. The geomagnetic storm on 21–22 January 2005 is considered to be anomalous as the SYM-H index that signifies the strength of ring current, decreases and had a sustained trough value of −101 nT lasting more than 6 hr under northward IMF Bz conditions. In this work, the standard WINDMI model is utilized to estimate the growth and decay of magnetospheric currents by using several solar wind-magnetosphere coupling functions. However, it is found that the WINDMI model driven by any of these coupling functions is not fully able to explain the decrease of SYM-H under northward IMF Bz. A dense plasma sheet along with signatures of a highly stretched magnetosphere was observed during this storm. The SYM-H variations during the entire duration of the storm were only reproduced after modifying the WINDMI model to account for the effects of the dense plasma sheet. The limitations of directly driven models relying purely on the solar wind parameters and not accounting for the state of the magnetosphere are highlighted by this work.