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\begin{document}

\title{Solar and magnetic control of minor ion peaks in the dayside Martian
ionosphere}



\author[1]{Jun Cui}%
\author[2]{Jianping Huang}%
\author[3]{Yongqiang Hao}%
\author[4]{Jianpeng Guo}%
\author[5]{Xiaoshu Wu}%
\author[6]{Dandan Niu}%
\author[7]{Yong Wei}%
\affil[1]{Sun Yat-sen University}%
\affil[2]{Sun Yat-Sen University}%
\affil[3]{Peking University}%
\affil[4]{Beijing Normal University}%
\affil[5]{National Astronomical Observatories, Chinese Academy of Sciences}%
\affil[6]{Macau University of Science and Technology}%
\affil[7]{Institute of Geology and Geophysics, Chinese Academy of Sciences}%


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  \date{May 25, 2024}


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\begin{abstract}
The Neutral Gas and Ion Mass Spectrometer of the Mars Atmosphere and
Volatile Evolution provides a large data set to explore the ion
composition and structure of the Martian ionosphere. Here the dayside
measurements are used to investigate the minor ion density profiles with
distinctive peaks above 150 km, revealing a systematic trend of
decreasing peak altitude with increasing ion mass. We specifically focus
on a subset of species including O\$\^{}+\$, N\$\_2\^{}+\$/CO\$\^{}+\$,
C\$\^{}+\$, N\$\^{}+\$, He\$\^{}+\$, and O\$\^{}\{++\}\$, all of which
are mainly produced via direct photoionization of parent neutrals. Our
analysis reveals weak or no variation with solar zenith angle (SZA) in
both peak density and altitude, which is an expected result because
these ion peaks are located within the optically thin regions subject to
the same level of solar irradiance independent of SZA. In contrast, the
solar cycle variations of peak density and altitude increase
considerably with increasing solar activity, as a result of enhanced
photoionization frequency and atmospheric expansion at high solar
activities. He\$\^{}+\$ serves as an exception in that its peak density
increases towards large SZA and meanwhile shows no systematic variation
with solar activity. The thermospheric He distribution on Mars should
play an important role in determining these observed variations.
Finally, the peak altitudes for all species are elevated by at least
several km within the weakly magnetized regions, possibly attributable
to the suppression of vertical diffusion by preferentially horizontal
magnetic fields in these regions.%
\end{abstract}%



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