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Revealing the Intensity of Turbulent Energy Transfer in Planetary Atmospheres
Author(s) -
Cabanes Simon,
Espa Stefania,
Galperin Boris,
Young Roland M. B.,
Read Peter L.
Publication year - 2020
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2020gl088685
Subject(s) - turbulence , physics , atmosphere (unit) , atmosphere of jupiter , planet , jupiter (rocket family) , saturn , intensity (physics) , atmospheric sciences , astrophysics , astronomy , meteorology , jovian , optics , space shuttle
Abstract Images of the giant planets Jupiter and Saturn show highly turbulent storms and swirling clouds that reflect the intensity of turbulence in their atmospheres. Quantifying planetary turbulence is inaccessible to conventional tools, however, since they require large quantities of spatially and temporally resolved data. Here we show, using experiments, observations, and simulations, that potential vorticity (PV) is a straightforward and universal diagnostic that can be used to estimate turbulent energy transfer in a stably stratified atmosphere. We use the conservation of PV to define a length scale, L M , representing a typical distance over which PV is mixed by planetary turbulence. L M increases as the turbulent intensity increases and can be estimated from any latitudinal PV profile. Using this principle, we estimate L M within Jupiter's and Saturn's tropospheres, showing for the first time that turbulent energy transfer in Saturn's atmosphere is four times less intense than Jupiter's.