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\begin{document}

\title{Convective vortices and dust devils detected and characterized by Mars
2020}



\author[1]{Ricardo Hueso}%
\author[2]{Claire Newman}%
\author[3]{Teresa del Rio-Gaztelurrutia}%
\author[1]{Asier Munguira}%
\author[4]{Agustín Sánchez-Lavega}%
\author[5]{Daniel Toledo}%
\author[6]{Víctor Apéstigue}%
\author[7]{Ignacio Arruego}%
\author[8]{Alvaro Vicente-Retortillo}%
\author[9]{German Martinez}%
\author[10]{Mark T Lemmon}%
\author[11]{Ralph D. Lorenz}%
\author[2]{Mark Ian Richardson}%
\author[8]{Daniel Viúdez-Moreiras}%
\author[12]{Manuel de la Torre Juárez}%
\author[13]{Jose Antonio Rodríguez-Manfredi}%
\author[14]{Leslie Tamppari}%
\author[15]{Naomi Murdoch}%
\author[13]{Sara Navarro López}%
\author[16]{Javier Gomez-Elvira}%
\author[17]{Mariah Baker}%
\author[18]{Jorge Pla-García}%
\author[19]{Ari-Matti Harri}%
\author[19]{Maria Hieta}%
\author[19]{Maria Genzer}%
\author[19]{Jouni Polkko}%
\author[19]{Iina Jaakonaho}%
\author[19]{Teemu J T Mäkinen}%
\author[15]{Alexander Stott}%
\author[20]{David Mimoun}%
\author[21]{Baptiste Chide}%
\author[13]{Eduardo Sebastian Martínez}%
\author[22]{Donald Banfield}%
\author[23]{Alain Lepinette Malvitte}%
\affil[1]{UPV/EHU}%
\affil[2]{Aeolis Research}%
\affil[3]{Universidad País Vasco UPV/EHU}%
\affil[4]{Universidad del Pais Vasco UPV/EHU}%
\affil[5]{Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain.}%
\affil[6]{National Institute of Aerospace Technology (INTA)}%
\affil[7]{INTA}%
\affil[8]{Centro de Astrobiología (INTA-CSIC)}%
\affil[9]{Lunar and Planetary Institute}%
\affil[10]{Space Science Institute}%
\affil[11]{Johns Hopkins University Applied Physics Lab}%
\affil[12]{Jet Propulsion Laboratory- California Institute of Technology, Pasadena, CA, USA}%
\affil[13]{Centro de Astrobiología}%
\affil[14]{Jet Propulsion Laboratory}%
\affil[15]{ISAE SUPAERO}%
\affil[16]{Centro de Astrobiologia}%
\affil[17]{Smithsonian Institution}%
\affil[18]{Centro de Astrobiología (CSIC-INTA)}%
\affil[19]{Finnish Meteorological Institute}%
\affil[20]{ISAE, INSTITUT SUPERIEUR DE L'AERONAUTIQUE ET DE L'ESPACE}%
\affil[21]{Los Alamos National Laboratory}%
\affil[22]{Cornell}%
\affil[23]{Centro de Astrobiologia, INTA-CSIC}%


\vspace{-1em}



  
  \date{May 25, 2024}


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\selectlanguage{english}
\begin{abstract}
We characterize the vortex and dust devil activity at Jezero from
pressure and winds obtained with the MEDA instrument on Mars 2020 over
415 sols (Ls=6-213\selectlanguage{ngerman}º). Vortices are abundant (4.9 vortices per sol with
pressure drops \textgreater{}0.5 Pa when correcting from gaps in
coverage) and peak at noon. At least one in every 5 vortices carries
dust from RDS-MEDA data, and intense vortices are more likely to carry
dust. Seasonal variability was small but dust devils were abundant
during a dust storm (Ls=152-156º). Vortices are more frequent and
intense over terrains with lower thermal inertia favoring a higher
daytime surface-to-air temperature gradient. We fit measurements of wind
and pressure during dust devil encounters to models of vortices, and
investigate their physical characteristics. Diameters range from 5 to
135 m with a mean of 20 m. Three 100-m size events passed within 30 m of
the rover. From the close encounters we estimate a dust devil activity
of 2.0-3.0 dust devils km\$\^{}\{-2\}\$ sol\$\^{}\{-1\}\$. A comparison
of MEDA observations with a Large Eddy Simulation of Jezero at Ls=45º
produces a similar result. We estimate that large dust devils with
diameters \$\textgreater{}100\$ m have a density of 0.1 dust devils
km-2sol-1, implying that dust lifting is dominated by the largest
vortices in the region. At least one vortex had a central pressure drop
of 9.0 Pa and internal winds of 25 ms-1. The MEDA wind sensors were
partially damaged during two dust devil encounters, and we detail these
events.%
\end{abstract}\selectlanguage{ngerman}%



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