# Io's dry body shaped by atmospheric instability

Olivier Mousis, Emmanuel Marcq, Artyom Aguichine, François Leblanc, Kathleen Mandt, Antoine Schneeberger, Martin Turbet

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Olivier Mousis, Emmanuel Marcq, Artyom Aguichine, François Leblanc, Kathleen Mandt, et al. Io's dry body shaped by atmospheric instability. European Planetary Science Congress. EPSC 2021, Sep 2021, Virtual Meeting, France. pp.306-322, 10.5194/epsc2021-187. insu-03313836

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Submitted on 4 Aug 2021

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# Io's dry body shaped by atmospheric instability

Olivier Mousis<fnref n="1" />, Emmanuel Marcq<fnref n="2" />, Artyom Aguichine<fnref n="1" />, François Leblanc<fnref n="2" />, Kathleen Mandt<fnref n="3" />, Antoine Schneeberger<fnref n="1" />, and Martin Turbet<fnref n="4" />

One of the outstanding questions regarding the architecture of the Galilean moons system is the nature of the processes that shaped its density gradient, which results from the fact that Ganymede and Callisto share an ice-to-rock ratio close to unity while Io and Europa are heavily depleted in volatiles. Two categories of scenarios, gathered in two distinct phases of moons formation and evolution, have been proposed to account for this density gradient in the literature: either the building blocks of the two innermost moons Io and Europa have been depleted in volatiles during their migration in the hot part of the Jovian circumplanetary disk [1-3], or they initially accreted ice-rich building blocks in a colder environment. In this case, their primitive oceans would have mostly vanished via hydrodynamic escape due to the high accretional energy [4].

<footnote n="1">¹Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France</footnote>

<footnote n="2">²LATMOS/IPSL, UVSQ, Université Paris-Saclay, Sorbonne Université, CNRS, Guyancourt, France</footnote>

<footnote n="3">³Johns Hopkins University Applied Physics Laboratory, 240-592-0262, Laurel, MD, USA</footnote>

<footnote n="4">⁴Observatoire astronomique de l'Université de Genève, 51 chemin des Maillettes, Switzerland</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Thickness of Io's primitive atmosphere (in units of satellite radius) expressed as a function of pressure (in units of surface pressure) for several temperatures.</figcaption></figure>

Here, we investigate the possibility that Io also accreted from water-rich building blocks and that its hydrosphere vanished because of hydrostatic instability, i.e. when the gravity at a given height is insufficient to retain gas. Io's putative primordial atmosphere would be either situated atop of a magma mantle, or a coexisting liquid ocean, depending on the surface temperature and pressure. To do so, we use the atmosphere model elaborated by [5,6] in which the properties of a 1D spherical atmosphere of water are generated by integrating the thermodynamic profiles bottom to top. The model takes as inputs the satellite's mass and radius, as well as the thermodynamic conditions at its bottom. Figure 1 represents the atmosphere thickness as a function of surface pressure and temperature. It shows that atmospheric thicknesses higher than 10 Io's radii are reached for surface temperatures equal or higher than 1250 K, indicating that such H₂O-dominated atmospheres would be gravitationally unstable at those temperatures. Such high temperatures needed at the base of the atmosphere to favor hydrostatic instability could result from the combination of accretional heating and heating generated by greenhouse effect. If effective, this mechanism would naturally explain why Io is devoid in volatiles without the need of invoking pre-accretional formation scenarios.

[1] Canup, R.M. & Ward, W.R. 2002, AJ, 124, 3404. doi:10.1086/344684

[2] Mousis, O. & Gautier, D. 2004, PSS, 52, 361. doi:10.1016/j.pss.2003.06.004

[3] Ronnet, T., Mousis, O., & Vernazza, P. 2017, ApJ, 845, 92. doi:10.3847/1538-4357/aa80e6

[4] Bierson, C.J. & Nimmo, F. 2020, ApJL, 897, L43. doi:10.3847/2041-8213/aba11a
[5] Marcq, E., Salvador, A., Massol, H., et al. 2017, JGR (Planets), 122, 1539.
doi:10.1002/2016JE005224

[6] Marcq, E. 2012, JGR (Planets), 117, E01001. doi:10.1029/2011JE003912