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\begin{document}

\title{The growth of ring current/SYM-H under northward IMF \$B\_z\$ conditions
present during the 21-22 January 2005 geomagnetic storm}



\author[1]{Diptiranjan Rout}%
\author[2]{Swadesh Patra}%
\author[3]{Sandeep Kumar}%
\author[4]{Dibyendu Chakrabarty}%
\author[5]{Geoffrey D. Reeves}%
\author[6]{Claudia Stolle}%
\author[7]{Kuldeep Pandey}%
\author[8]{Shibaji Chakraborty}%
\author[9]{Edmund A. Spencer}%
\affil[1]{GFZ German Research Centre for Geosciences}%
\affil[2]{University of New Brunswick}%
\affil[3]{Institute for Space-Earth Environmental Research, Nagoya University}%
\affil[4]{Physical Research Laboratory}%
\affil[5]{Space Science and Applications Group, Los Alamos National Laboratory, Los Alamos, New Mexico, USA.}%
\affil[6]{Leibniz Institut of Atmosphereic Physics at the University of Rostock}%
\affil[7]{University of Saskatchewan}%
\affil[8]{Virginia Tech}%
\affil[9]{University of South Alabama}%


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  \date{June 16, 2024}


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\begin{abstract}
The total energy transfer from the solar wind to the magnetosphere is
governed by the reconnection rate at the magnetosphere edges as the IMF
\$B\_z\$ turns southward. The delayed response of the ring current to
solar wind driving can account for the anomalous growth of the SYM-H
under northward IMF \$B\_z\$. 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, grows and has a sustained peak value lasting
more than 6 hrs under northward IMF \$B\_z\$ conditions. In this work,
first the standard WINDMI model is utilized to estimate the growth and
decay of various magnetospheric currents by using several solar
wind-magnetopsehre coupling functions. However, it is found that the
WINDMI model driven by any of these coupling functions is not fully able
to explain the enhancement of SYM-H under northward IMF \$B\_z\$. The
SYM-H variations during the entire duration of the storm were only
reproduced when the effects of the dense plasma sheet were included in
the WINDMI model. 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.%
\end{abstract}%



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