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\begin{document}

\title{Analytical assessment of Kelvin-Helmholtz instability growth at
Ganymede's upstream magnetopause}



\author[1]{Nawapat Kaweeyanun}%
\author[1]{Adam Masters}%
\author[2]{Xianzhe Jia}%
\affil[1]{Imperial College London}%
\affil[2]{University of Michigan-Ann Arbor}%


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  \date{June 18, 2024}


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\begin{abstract}
Ganymede is the only Solar System moon that generates a permanent
magnetic field. Dynamics inside Ganymede's magnetosphere is likely
driven by energy-transfer interactions on its upstream magnetopause.
Previously in Kaweeyanun et al. (2020), we created a steady-state
analytical model of Ganymede's magnetopause and predicted global-scale
magnetic reconnection to occur frequently throughout the surface. Using
the same model, this paper provides the first assessment of
Kelvin-Helmholtz (K-H) instability growth on the magnetopause in
isolation from reconnection effects. The linear K-H instability growth
rate is calculated at Ganymede's equatorial magnetopause flank points
under the magnetohydrodynamic with finite Larmor radius effect (MHD-FLR)
theory, which accounts for inter-flank growth rate asymmetry due to
large gyroradii of Jovian plasma ions. The calculation gives growth
rates between \selectlanguage{greek}γ \selectlanguage{english}[?] \selectlanguage{english}0.01-48 /s with notable enhancement at the equatorial
flank point closer to Jupiter. Then, the ideal MHD K-H instability onset
condition is evaluated across the entire Ganymedean magnetopause. We
find the conditions along both magnetopause flanks to be K-H favorable
at all latitudes with growth rates similar to those at respective
equatorial flank points. Using Mercury's magnetopause case as a
comparison, we determined that nonlinear K-H vortices are viable at
Ganymede based on the calculated growth rates, but the vortex growth
will likely be suppressed once global reconnection is taken into
account.%
\end{abstract}%



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