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\begin{document}

\title{Plasma Mixing during active Kelvin-Helmholtz Instability under different
IMF orientations}



\author[1]{Adriana Settino}%
\author[1]{Rumi Nakamura}%
\author[2]{Kevin Alexander Blasl}%
\author[3]{Daniel Bruce Graham}%
\author[4]{Takuma Nakamura}%
\author[5]{Owen Roberts}%
\author[6]{Zoltan Vörös}%
\author[2]{Evgeny V. Panov}%
\author[7]{Cyril L. Simon Wedlund}%
\author[8]{Daniel Schmid}%
\author[2]{Martin Hosner}%
\author[7]{Martin Volwerk}%
\author[3]{Yuri V. Khotyaintsev}%
\affil[1]{Space Research Institute}%
\affil[2]{Space Research Institute, Austrian Academy of Sciences}%
\affil[3]{Swedish Institute of Space Physics}%
\affil[4]{Institute of Physics, University of Graz}%
\affil[5]{IWF}%
\affil[6]{Space Research Institute, Austrian Academy of Sciences, 8042 Graz, Austria}%
\affil[7]{Space Research Institute, OEAW}%
\affil[8]{Space Research Institute Graz (IWF), Austrian Academy of Sciences (OeAW)}%


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  \date{May 18, 2024}


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\selectlanguage{english}
\begin{abstract}
When the velocity shear between the two plasmas separated by Earth's
magnetopause is locally super-Alfv\selectlanguage{ngerman}énic, the Kelvin-Helmholtz (KH)
instability can develop. A crucial role is played by the interplanetary
magnetic field (IMF) orientation, which can stabilize the velocity
shear. Although, in a linear regime, the instability threshold is
equally satisfied during both northward and southward IMF orientations,
in-situ measurements show that KH instability is preferentially excited
during the northward IMF orientation. We investigate this different
behavior by means of a mixing parameter which we apply to two KH events
to identify both boundaries and the center of waves/vortices. During the
northward orientation, the waves/vortex boundaries have stronger
electrons than ions mixing, while the opposite is observed at their
center. During the southward orientation, instead, particle mixing is
observed predominantly at the boundaries. In addition, stronger local
ion and electron non-thermal features are observed during the northward
than the southward IMF orientation. Specifically, ion distribution
functions are more distorted, due to field-aligned beams, and electrons
have a larger temperature anisotropy during the northward than the
southward IMF orientation. The observed kinetic features provide an
insight into both local and remote processes that affect the evolution
of KH structures.%
\end{abstract}\selectlanguage{ngerman}%



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