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\begin{document}

\title{Atmospheric Escape Processes and Planetary Atmospheric Evolution}



\author[1]{Guillaume Gronoff}%
\author[2]{Phil Arras}%
\author[3]{Suleiman M Baraka}%
\author[4]{Jared M Bell}%
\author[5]{Gaël Cessateur}%
\author[6]{Ofer Cohen}%
\author[7]{Shannon M. Curry}%
\author[6]{Jeremy J Drake}%
\author[8]{Meredith K Elrod}%
\author[9]{Justin T. Erwin}%
\author[8]{Katherine Garcia-Sage}%
\author[10]{Cecilia garraffo}%
\author[4]{Alex Glocer}%
\author[11]{Nicholas Gray Heavens}%
\author[11]{Kylie Lovato}%
\author[12]{Romain Maggiolo}%
\author[13]{Christopher D. Parkinson}%
\author[14]{Cyril L. Simon Wedlund}%
\author[15]{Daniel R Weimer}%
\author[11]{William B. Moore}%
\affil[1]{Nasa LaRC}%
\affil[2]{Univerity of Virginia}%
\affil[3]{Al-Aqsa University}%
\affil[4]{NASA/GSFC}%
\affil[5]{Belgian Institute for Space Aeronomy (IASB-BIRA)}%
\affil[6]{Harvard-Smithsonian Center for Astrophysics}%
\affil[7]{UC Berkeley}%
\affil[8]{NASA Goddard Space Flight Center}%
\affil[9]{University of Arizona}%
\affil[10]{Harvard-Smithsonian Center for Astrophysics,}%
\affil[11]{Hampton University}%
\affil[12]{Belgian royal Institute for Space Aeronomy (IASB-BIRA)}%
\affil[13]{University of Michigan-Ann Arbor}%
\affil[14]{Space Research Institute}%
\affil[15]{Virginia Tech}%


\vspace{-1em}



  
  \date{May 17, 2024}


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\begin{abstract}
The habitability of the surface of any planet is determined by a complex
evolution of its interior, surface, and atmosphere. The electromagnetic
and particle radiation of stars drive thermal, chemical and physical
alteration of planetary atmospheres, including escape. Many known
extrasolar planets experience vastly different stellar environments than
those in our Solar system: it is crucial to understand the broad range
of processes that lead to atmospheric escape and evolution under a wide
range of conditions if we are to assess the habitability of worlds
around other stars. One problem encountered between the planetary and
the astrophysics communities is a lack of common language for describing
escape processes. Each community has customary approximations that may
be questioned by the other, such as the hypothesis of H-dominated
thermosphere for astrophysicists, or the Sun-like nature of the stars
for planetary scientists. Since exoplanets are becoming one of the main
targets for the detection of life, a common set of definitions and
hypotheses are required. We review the different escape mechanisms
proposed for the evolution of planetary and exoplanetary atmospheres. We
propose a common definition for the different escape mechanisms, and we
show the important parameters to take into account when evaluating the
escape at a planet in time. We show that the paradigm of the magnetic
field as an atmospheric shield should be changed and that recent work on
the history of Xenon in Earth's atmosphere gives an elegant explanation
to its enrichment in heavier isotopes: the so-called Xenon paradox.%
\end{abstract}%



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