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Emergence of polar-jet polygons from jet instabilities in a Saturn model

Morales-Juberías, Raúl and Sayanagi, Kunio M. and Dowling, Timothy E. and Ingersoll, Andrew P. (2010) Emergence of polar-jet polygons from jet instabilities in a Saturn model. Icarus, 211 (2). pp. 1284-1293. ISSN 0019-1035. https://resolver.caltech.edu/CaltechAUTHORS:20110309-164547697

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Abstract

Voyager flybys of Saturn in 1980–1981 revealed a circumpolar wave at ≈78° north planetographic latitude. The feature had a dominant wavenumber 6 mode, and has been termed the Hexagon from its geometric appearance in polar-projected mosaics. It was also noted for being stationary with respect to Saturn’s Kilometric Radiation (SKR) rotation rate. The Hexagon has persisted for over 30 years since the Voyager observations until now. It has been observed from ground based telescopes, Hubble Space Telescope and multiple instruments onboard Cassini in orbit around Saturn. Measurements of cloud motions in the region reveal the presence of a jet stream whose path closely follows the Hexagon’s outline. Why the jet stream takes the characteristic six-sided shape and how it is stably maintained across multiple saturnian seasons are yet to be explained. We present numerical simulations of the 78.3°N jet using the Explicit Planetary Isentropic-Coordinate (EPIC) model and demonstrate that a stable hexagonal structure can emerge without forcing when dynamic instabilities in the zonal jet nonlinearly equilibrate. For a given amplitude of the jet, the dominant zonal wavenumber is most strongly dependent on the peak curvature of the jet, i.e., the second north–south spatial derivative of the zonal wind profile at the center of the jet. The stable polygonal shape of the jet in our simulations is formed by a vortex street with cyclonic and anticyclonic vortices lining up towards the polar and equatorial side of the jet, respectively. Our result is analogous to laboratory experiments of fluid motions in rotating tanks that develop polygonal flows out of vortex streets. However, our results also show that a vortex street model of the Hexagon cannot reproduce the observed propagation speed unless the zonal jet’s speed is modified beyond the uncertainties in the observed zonal wind speed, which suggests that a vortex street model of the Hexagon and the observed zonal wind profile may not be mutually compatible.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1016/j.icarus.2010.11.006DOIArticle
ORCID:
AuthorORCID
Sayanagi, Kunio M.0000-0001-8729-0992
Ingersoll, Andrew P.0000-0002-2035-9198
Additional Information:© 2010 Elsevier Inc. Received 23 April 2010; revised 2 November 2010; accepted 4 November 2010. Available online 17 November 2010. We acknowledge Tim Mattox for his help with the setup of the parallel cluster RAVEN on which some of these simulations were carried out. Computational resources were also provided by the New Mexico Computing Applications Center and New Mexico Institute of Mining and Technology. This work was supported by NASA Planetary Atmospheres Grant numbers NNX08AE91G (NMT), NNG05GO06Gd and NNX08AE64G (UofL).
Funders:
Funding AgencyGrant Number
NASANNX08AE91G
NASANNG05GO06Gd
NASANNX08AE64G
Subject Keywords:Jovian planets; Saturn, Atmosphere; Atmospheres, Dynamics
Issue or Number:2
Record Number:CaltechAUTHORS:20110309-164547697
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110309-164547697
Official Citation:Raul Morales-Juberias, Kunio M. Sayanagi, Timothy E. Dowling, Andrew P. Ingersoll, Emergence of polar-jet polygons from jet instabilities in a Saturn model, Icarus, Volume 211, Issue 2, February 2011, Pages 1284-1293, ISSN 0019-1035, DOI: 10.1016/j.icarus.2010.11.006. (http://www.sciencedirect.com/science/article/B6WGF-51GRWJK-2/2/379a461f9d2f47709e16d1cd13966a59)
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22789
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:10 Mar 2011 18:58
Last Modified:09 Mar 2020 13:19

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