A long-lived cyclone in Saturn’s atmosphere: Observations and models

Río‐Gaztelurrutia, T. del; Legarreta, J.; Hueso, R.; Pérez‐Hoyos, S.; Sánchez‐Lavega, A.

doi:10.1016/j.icarus.2010.04.002

Cited by 19 publications

(17 citation statements)

References 44 publications

(78 reference statements)

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“…While the height of the tropospheric haze is in good agreement with the results of Río-Gaztelurrutia et al (2010), our retrieved cloud heights are considerably deeper than the roughly 350 mbar cloud tops they inferred.…”

Section: Cyclonesupporting

confidence: 89%

“…Both profiles show a clear trend towards a maximum in this pressure level at the center of the vortex, ranging from an average pressure of about 130 mbar to 150 mbar along the rim to a maximum pressure of about 175 mbar a the center of the vortex. This corresponds to a height difference of ~5km from the center to the edge of the roughly 1850 ± 180 km by 860 ± 90 km cyclone (Río-Gaztelurrutia et al, 2010). This is consistent with this being a region of downwelling aloft, as is expected for a cyclone in Saturn's upper troposphere.…”

Section: Cyclonesupporting

confidence: 81%

“…This long-lived feature has been previously analyzed by Río-Gaztelurrutia et al (2010), who investigated the vertical structure as well as the winds and dynamics.…”

Section: Cyclonementioning

confidence: 97%

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Saturn’s cloud structure inferred from Cassini ISS

Roman

Banfield

Gierasch

2013

Icarus

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Using high-resolution Cassini ISS images with wavelengths ranging from the ultraviolet to the near infrared, we have retrieved Saturn's atmospheric aerosol structure and properties for a broad range of latitudes in the southern hemisphere. The observations are consistent with two distinct layers of haze. Each layer is characterized by a vertical location, an optical depth, and a mean particle size, all of which vary with latitude. The tropospheric haze is optically thickest and extends to the greatest heights (~40 mbar) over the equator; its top surface is at significantly greater depths (~150 mbar ) at mid-latitudes. The height of the haze correlates well with position of the tropopause as indicated by the temperature field. Beneath this haze, we find a scattered denser cloud responsible for small-scale contrasts at an average depth of 1.75 ± 0.4 bar, with some features deeper than 2.5 bar.iii BIOGRAPHICAL SKETCHMichael Roman transferred into Cornell University in 2004 as a junior in the field of Atmospheric Sciences, after having studied at a small community college. As an undergraduate, he became involved in research as a student research assistant, organizing and processing image data from the Galileo mission. The project combined two of his of long-lived interest-meteorology and astronomy-and encouraged him to pursue further research experience.

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Section: Cyclonesupporting

confidence: 89%

Section: Cyclonesupporting

confidence: 81%

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Saturn’s cloud structure inferred from Cassini ISS

Roman

Banfield

Gierasch

2013

Icarus

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“…The zonal wind profile at 0. v uPmPP = is a non-dimensional vertical amplitude factor. We tested different values for slope m above and below P 0 = 500 mbar [27][28] . Similarly, for the thermal structure we adopted N(P) increasing with altitude for P<500 mbar 26 and …”

mentioning

confidence: 99%

Deep winds beneath Saturn’s upper clouds from a seasonal long-lived planetary-scale storm

Sánchez‐Lavega

Río‐Gaztelurrutia²,

Hueso³

et al. 2011

Nature

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“…A survey of Cassini ISS images shows that a system of three vortices formed in this latitudinal region in 2012 and has remained active until present, confirming that vortices in Saturn can be long lived [2]. In May 2015 a disturbance started to develop at the location of the triple vortex.…”

Section: Introductionmentioning

confidence: 80%

A planetary-scale disturbance in a long living three vortex coupled system in Saturn's atmosphere

Río‐Gaztelurrutia¹,

Sánchez‐Lavega²,

Antuñano³

et al. 2018

Icarus

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The zonal wind profile of Saturn has a singular structure in the latitude range 50ºN-65ºN planetocentric, with a double peak that reaches maximum zonal velocities close to 100ms -1 [1]. A survey of Cassini ISS images shows that a system of three vortices formed in this latitudinal region in 2012 and has remained active until present, confirming that vortices in Saturn can be long lived [2]. In May 2015 a disturbance started to develop at the location of the triple vortex. Since at the time Cassini orbits were not favorable to the observation of the region, we were granted Director Discretionary Time of the Hubble Space Telescope to observe the region before the perturbation faded away. Here we report the dynamics and vertical structure of the three-vortex system and of the disturbance that developed at its location, based on HST and Cassini images. We also present results of numerical models to explain the stability of vortices in the region.

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A long-lived cyclone in Saturn’s atmosphere: Observations and models

Cited by 19 publications

References 44 publications

Saturn’s cloud structure inferred from Cassini ISS

Saturn’s cloud structure inferred from Cassini ISS

Deep winds beneath Saturn’s upper clouds from a seasonal long-lived planetary-scale storm

A planetary-scale disturbance in a long living three vortex coupled system in Saturn's atmosphere

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