Title: Étude de la composition et de la dynamique des planètes géantes : Préparation de la mission JUICE
Scientific context: Observe the atmosphere of Jupiter and the other giant planets (comparative planetology) with earth- and space-based facilities (e.g. Odin, ALMA) to characterize their composition and dynamics, in preparation of the JUICE mission (see this post) and the science investigations of SWI (see this post).
Student: Vincent Hue (currently Research Scientist at SwRI, San Antonio, TX, USA)
Title: “Modélisation physico-chimique 3D des atmosphères des planètes géantes”
Supervisors: M. Dobrijevic, F. Hersant, and T. Cavalié
Scientific Context: Long-term and spatially-resolved observations of the giant planets with Cassini and ALMA
Objective: Develop a 2D seasonal photochemical model of the giant planets to interpret the spatially-resolved observations
Results: The model solves the continuity equation for all altitudes (~H/3 resolution), latitudes (5° resolution) and as a funtion of time (10° heliocentric longitude resolution). The chemical network contains 22 species, 33 reactions and 24 photodissociations. The temporal evolution of the solar declination is computed from the orbital parameters (period, eccentricity, obliquity, etc.). The actiinic flux is computed with a 3Dspherical geometry radiative transfer model. The model can be fed with a seasonal altitude-latitude thermal field either coming from observations or simulated with a GCM ( general circulation model). The vertical and horizontal eddy mixing (Kyy and Kzz) and advective transport are implemented. Finally, the ring shadowing for Saturn is taken into account.
Acetylene and ethane in the stratosphere of Saturn, as a function of latitude. Comparison of model outputs with observations (taken from Hue et al. 2015).
Publications linked to the projet:
Hue, V., Hersant, F., Cavalié, T., Dobrijevic, M., 2018. Photochemistry, mixing and transport in Jupiter’s stratosphere constrained by Cassini. Icarus 307, 106-123 .
Hue, V., Greathouse, T. K., Cavalié, T., Dobrijevic, M., Hersant, F., 2016. 2D photochemical modeling of Saturn’s stratosphere. Part II: Feedback between composition and temperature. Icarus 267, 334-343.
Hue, V., Cavalié, T., Dobrijevic, M., Hersant, F., Greathouse, T. K., 2015. 2D photochemical modelling of Saturn’s stratosphere. Part I: Seasonal variation of atmospheric composition. Icarus 257, 163-184.
Cavalié, T., Dobrijevic, M, Fletcher, L. N., Loison, J. C., Hickson, K. M., Hue, V., Hartogh, P., 2015. The photochemical response to the variation of temperature in Saturn’s 2011-2012 stratospheric vortex. Astronomy and Astrophysics 580, A55.
Dobrijevic, M., Cavalié, T., Billebaud, F., 2011. A methodology to construct a reduced chemical scheme for 2D-3D photochemical models: Application to Saturn. Icarus 214, 275-285.
The detection of water in the upper atmospheres (i.e. stratospheres) of the giant planets by the Infrared Space Observatory (ISO ; Feuchtgruber et al. 1997) raised the question of its origin. The cold trap at the tropopause of these planets prevents efficient transport of water from the planetary interiors (supposed to be water-rich) to the stratospheres because of condensation. The water observed by ISO is then external and results from the ablation of micrometeoroids from interplanetary dust or icy ring/satellite particles or from large comet impacts. While Jupiter’s stratospheric water is due to the Shoemaker-Levy 9 impacts in 1994 (refer to this post), the situation at Saturn remained unclear.
The Cassini mission detected water plumes at the South Pole of Enceladus, one of Saturn’s small moons, in 2006 (Porco et al. 2006, Waite et al. 2006, Hansen et al. 2006). Water then forms a torus at 4 Saturn radii, the orbital distance of Enceladus, as proved by the first observations of Saturn with the Herschel Space Observatory (Hartogh et al. 2011 ; refer to this post). Models then predicted that a fraction of this water would rain onto Saturn’s atmosphere (e.g. Cassidy and Johnson 2010), but a confirmation from direct observation was missing.
This missing piece came from Herschel mapping observations carried out in 2010-2011 with the PACS (Photodetector Array Camera and Spectrometer) instrument. The analysis of the data demonstrate that the meridional distribution of water in Saturn’s stratosphere is not uniform (as would be expected from interplanetary dust particles or an ancient comet impact): it peaks at the equator and can be modelled with a gaussian decrease towards the poles, with a half-width-at-half-maximum of 25° in latitude. This is consistent with model prediction and shows that a fraction of the water delivered by the Enceladus plumes eventually falls onto Saturn’s stratosphere
During its final orbits, Cassini detected an extraordinary influx of material coming from the ring plane (Waite et al. 2018, Perry et al. 2018). This influx is orders of magnitude stronger than the one originating from the Enceladus plumes. It seems to be quite recent and needs confirmation from new observations.
Reference: Cavalié et al. 2019, Astronomy and Astrophysics 630, A87.