Saturn’s zonal wind profile in 2004–2009 from Cassini ISS images and its long-term variability

• Published in: Icarus (New York, N.Y. 1962) Vol. 215; no. 1; pp. 62 - 74
• Main Authors: García-Melendo, E., Pérez-Hoyos, S., Sánchez-Lavega, A., Hueso, R.
• Format: Journal Article
• Language: English
• Published: Amsterdam Elsevier Inc 01.09.2011; Elsevier
• Subjects: Astronomy; Atmospheres, Dynamics; Earth, ocean, space; Exact sciences and technology; Saturn, Atmosphere; Solar system; Saturn, Atmosphere; Atmospheres, Dynamics; Methane; Shear; Wind field; Zonal wind; Northern hemisphere; Intensity; Variability; Shading; Long term variation; Southern hemisphere; Continuum; Saturn planet; Dynamics; Jets; Solar system
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2011.07.005

► We retrieved Saturn’s winds from ISS Cassini CB and MT images from 2004 to 2009. ► Differences between CB and MT zonal winds are due to vertical thermal wind shear. ► We supply tabular data of the ISS Cassini CB and MT Cassini wind profiles. ► Outside the equator zonal winds have remained stable during a complete Saturn’s year. ► There is a major change in the equatorial winds possibly after the 1990 GWS event. Five years of Cassini Imaging Science Subsystem images, from 2004 to 2009, are analyzed in this work to retrieve global zonal wind profiles of Saturn’s northern and southern hemispheres in the methane absorbing bands at 890 and 727 nm and in their respective adjacent continuum wavelengths of 939 and 752 nm. A complete view of Saturn’s global circulation, including the equator, at two pressure levels, in the tropopause (60 mbar to 250 mbar with the MT filters) and in the upper troposphere (from ∼350 mbar to ∼500 mbar with the CB filter set), is presented. Both zonal wind profiles (available at the Supplementary Material Section), show the same structure but with significant differences in the peak of the eastward jets and the equatorial region, including a region of positive vertical shear symmetrically located around the equator between the 10° < | φ c | < 25° where zonal velocities close to the tropopause are higher than at 500 mbar. A comparison of previously published zonal wind sets obtained by Voyager 1 and 2 (1980–1981), Hubble Space Telescope, and ground-based telescopes (1990–2004) with the present Cassini profiles (2004–2009) covering a full Saturn year shows that the shape of the zonal wind profile and intensity of the jets has remained almost unchanged except at the equator, despite the seasonal insolation cycle and the variability of Saturn’s emitted power. The major wind changes occurred at equatorial latitudes, perhaps following the Great White Spot eruption in 1990. It is not evident from our study if the seasonal insolation cycle and its associated ring shadowing influence the equatorial circulation at cloud level.