Multilayer hazes over Saturn’s hexagon from Cassini ISS limb images

A. Sánchez-Lavega (), A. García-Muñoz, T. Río-Gaztelurrutia, S. Pérez-Hoyos, J. F. Sanz-Requena, R. Hueso, S. Guerlet and J. Peralta
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A. Sánchez-Lavega: Universidad del País Vasco UPV/EHU
A. García-Muñoz: Technische Universität Berlin
T. Río-Gaztelurrutia: Universidad del País Vasco UPV/EHU
S. Pérez-Hoyos: Universidad del País Vasco UPV/EHU
J. F. Sanz-Requena: Universidad de Valladolid
R. Hueso: Universidad del País Vasco UPV/EHU
S. Guerlet: Sorbonne Universite, Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique, Ecole Normale Superieure (ENS)
J. Peralta: Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency

Nature Communications, 2020, vol. 11, issue 1, 1-8

Abstract: Abstract In June 2015, Cassini high-resolution images of Saturn’s limb southwards of the planet’s hexagonal wave revealed a system of at least six stacked haze layers above the upper cloud deck. Here, we characterize those haze layers and discuss their nature. Vertical thickness of layers ranged from 7 to 18 km, and they extended in altitude ∼130 km, from pressure level 0.5 bar to 0.01 bar. Above them, a thin but extended aerosol layer reached altitude ∼340 km (0.4 mbar). Radiative transfer modeling of spectral reflectivity shows that haze properties are consistent with particles of diameter 0.07–1.4 μm and number density 100–500 cm−3. The nature of the hazes is compatible with their formation by condensation of hydrocarbon ices, including acetylene and benzene at higher altitudes. Their vertical distribution could be due to upward propagating gravity waves generated by dynamical forcing by the hexagon and its associated eastward jet.

Date: 2020
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DOI: 10.1038/s41467-020-16110-1

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