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\begin{document}

\title{First observations of CH4 and H3+ equatorial detached layers, as seen by
JIRAM/Juno}



\author[1]{Alessandra Migliorini}%
\author[2]{Bianca Maria Dinelli}%
\author[3]{Chiara Castagnoli}%
\author[4]{Maria L. Moriconi}%
\author[1]{Francesca Altieri}%
\author[5]{Sushil K. Atreya}%
\author[6]{Alberto Adriani}%
\author[3]{Alessandro Mura}%
\author[3]{Federico Tosi}%
\author[3]{Alessandro Moirano}%
\author[1]{Giuseppe Piccioni}%
\author[1]{Davide Grassi}%
\author[6]{Roberto Sordini}%
\author[7]{Raffaella Noschese}%
\author[7]{Andrea Cicchetti}%
\author[8]{Scott J Bolton}%
\author[9]{Giuseppe Sindoni}%
\author[9]{Christina Plainaki}%
\author[9]{Angelo Olivieri}%
\affil[1]{INAF}%
\affil[2]{Istituto di Scienza dell'Atmosfera e del Clima - CNR}%
\affil[3]{INAF-IAPS}%
\affil[4]{CNR-ISAC}%
\affil[5]{University of Michigan-Ann Arbor}%
\affil[6]{IAPS-INAF}%
\affil[7]{Istituto Nazionale di Astrofisica}%
\affil[8]{Southwest Research Institute}%
\affil[9]{Agenzia Spaziale Italiana}%


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  \date{May 04, 2024}


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\begin{abstract}
In this work we present the detection of CH\textsubscript{4} and
H\textsubscript{3}\textsuperscript{+} emissions in the atmosphere of
Jupiter as two well separated layers, located, respectively, at a
tangent altitudes of about 200 km and 500-600 km above the 1-bar level.
We studied the vertical distribution of the two species retrieving their
Volume Mixing Ratio (VMR) and temperature simultaneously or allowing
only one quantity to vary. From this analysis, it is not possible to
firmly conclude if the observed H\textsubscript{3}\textsuperscript{+}
and CH\textsubscript{4} features are due to an increase of their VMR or
rather to variations of the temperature of the two molecules. However,
our retrieval indicates that CH\textsubscript{4} is in non-Local Thermal
Equilibrium (non-LTE) condition, considering that the retrieved
temperature values at about 300 km, where the maximum
CH\textsubscript{4} concentration lies, is always about 100 K higher
than the Galileo measurements.

We suggest that vertically propagating waves is the most likely
explanation for the observed VMR and temperature variations in the JIRAM
(Jovian InfraRed Auroral Mapper) data. Other possible phenomena could
explain the observed evidences, for example a dynamical activity driving
chemical species from lower layers towards the upper atmosphere, like
the advection-diffusion processes responsible for the enhancement
observed by Juno/MWR (MicroWave Radiometer), or soft electrons
precipitation, although a better modeling is required to confirm these
hypothesis.

The characterization of CH\textsubscript{4} and
H\textsubscript{3}\textsuperscript{+} species, simultaneously observed
by JIRAM, offers the opportunity for better constraining the atmospheric
models of Jupiter and understanding the planetary formation.%
\end{abstract}%



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