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\begin{document}

\title{Ionospheric Sluggishness: A Characteristic Time-Lag of the Ionospheric
Response to Solar Flares}



\author[1]{Shibaji Chakraborty}%
\author[1]{John Michael Ruohoniemi}%
\author[1]{Joseph Baker}%
\author[2]{Scott Bailey}%
\author[3]{Robyn Fiori}%
\author[4]{Kate Zawdie}%
\affil[1]{Virginia Tech}%
\affil[2]{Virginia Polytechnic Institute and State University}%
\affil[3]{Natural Resources Canada}%
\affil[4]{US Naval Research Laboratory}%


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  \date{May 26, 2024}


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\begin{abstract}
The term ``ionospheric sluggishness'' is used to describe the time delay
between maximum radio absorption in the ionosphere following the time of
maximum irradiance during a solar flare. Sluggishness is one of the
characteristic properties known to be maximized around D-region heights
and can be used for studying lower ionospheric (D-region) and
mesospheric chemistry. This article is our first attempt to estimate
ionospheric sluggishness using high frequency (HF, 3 -- 30 MHz)
instruments. Specifically, we report on first estimates of sluggishness
from riometer and SuperDARN observations following a solar flare and
propose two new methods to estimate sluggishness. Sluggishness is shown
to be anti-correlated with the peak solar X-ray flux and positively
correlated with solar zenith angle and geographic latitude. The choice
of instrument, method, and reference solar waveband effects the
sluggishness estimation. A simulation study was performed to estimate
the effective recombination coefficient, which was found to vary between
4-5 orders of magnitude. We suggest that the effective recombination
coefficient is highly sensitive to D-region's negative and positive ion
chemistry.%
\end{abstract}%



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