Why is jupiter layered

Water clouds form down at the densest layer of clouds. We have written many articles about Jupiter for Universe Today. Want more information on Jupiter? We have recorded a podcast just about Jupiter for Astronomy Cast. This raises some intriguing questions as to the physical origin of these features and might suggest either some missing physical processes in many models or inadequate spatial resolution.

Deep-rooted hot spots might offer one possible explanation, given the appearance of isolated vortical structures in some deep convection models e. The equatorial jets in all four giant planets pose other significant challenges to such models, for which the question remains unresolved as to whether these jets require a deep circulation e.

Yano et al. More generally the connection between shallow weather layers and deep-seated circulations and convection remains poorly understood. Deep models are currently unable to capture the complex structures of the weather layer while shallow weather layer models do not represent a physically realistic lower boundary.

This is a review article and readers are referred to the original cited references for the majority of material presented. Data relating to the Jupiter cloud winds used in Galperin et al. J Atmos Sci — Article Google Scholar. Nature — Science — Izv Vyssh Ucheb Zaved Matematika —5. Google Scholar. Icarus 1 — Geophys Res Lett —4. Icarus — Part III: Global statistical picture of zonostrophic turbulence in high-resolution 3D-turbulent simulations.

Icarus Cao H, Stephenson DJ Zonal flow magnetic field interaction in the semi-conducting region of giant planets. Charney JG Geostrophic turbulence. Davidson PA Turbulence: an introduction for scientists and engineers, 2nd edn.

Oxford Univ Press, Oxford. Book Google Scholar. Chapter Google Scholar. Geophys Res Lett — Dowling TE A relationship between potential vorticity and zonal wind on Jupiter. Int J Mod Phys Planet Sci J Fluids Frisch U Turbulence: the legacy of A. Cambridge University Press, Cambridge. Baltic Astron — Part I: evaluation of the radiative transfer model.

Explaining the Juno observations. J Geophys Res. Heimpel M, Gastine T, Wicht J Simulation of deep-seated zonal jets and shallow vortices in gas giant atmospheres. Nat Geosci — Hide R Dynamics of the atmospheres of the major planets. Phys Fluids — J Geophys Res — Cambridge University Press, pp — Springer-Praxis, Chichester, UK. Proc Natl Acad Sci — Lian Y, Showman AP Generation of equatorial jets by large-scale latent heating on the giant planets.

Liu J, Schneider T Mechanisms of jet formation on the giant planets. Liu J, Schneider T Convective generation of equatorial super rotation in planetary atmospheres. Liu J, Schneider T Scaling of off-equatorial jets in giant planet atmospheres. Rigid rotation. Astrophys J Pasadena, Jet Propulsion Laboratory, p Astron J Lett L J Atmos Sci 65 2 — I: zonal-mean circulation from Cassini and Voyager 1 data.

Q J R Meteorol Soc — Planet Space Sci — Nonlinear Proc Geophys — Rhines PB Waves and turbulence on a beta-plane. J Fluid Mech — Salmon R Baroclinic instability and geostrophic turbulence. Geophys Astrophys Fluid Dyn — Scott RB, Wang F Direct evidence of an oceanic inverse kinetic energy cascade from satellite altimetry. J Phys Oceanogr — Showman AP Numerical simulations of forced shallow-water turbulence: effects of moist convection on the large-scale circulation of Jupiter and Saturn.

J Atmos Sci Part II: multi-annual high-resolution dynamical simulations. Part II: analysis of eddy transports. Sukoriansky S, Galperin B, Dikovskaya N Universal spectrum of two dimensional turbulence on a rotating sphere and some basic features of atmospheric circulation on giant planets. Phys Rev Lett 89 12 Atmosphere 10 12 Vallis GK Atmospheric and oceanic fluid dynamics—fundamentals and large-scale circulation, 2nd edn.

Rep Prog Phys — Williams GP Planetary circulations: 1. Barotropic representation of Jovian and terrestrial turbulence. Williams GP Planetary circulations: 2. The Jovian quasi—geostrophic regimes. Williams GP Jovian and comparative atmospheric modeling.

Adv Geophys 28A— Williams GP Jovian dynamics. Part II: the genesis and equilibration of vortex sets. You might also be interested in: A Look at the Inside of Jupiter The Giant planets do not have the same kind of layers inside that the earth-like planets do. The history of the giant planets was so different that they formed with much more gas on the inside. The Poles of Jupiter and its Moons Jupiter has interesting poles. The poles of some of its large moons are interesting too.

Io is one of the big moons. Io has volcanoes near its poles! The other big moons are covered with ice, like Earth's Heat from Inside Jupiter Have you ever thought that a planet could make energy within itself? If you think about it, the ground is not very cold at all except in the winter.

This means that the Earth makes enough energy for Motions in Jupiter's Interior, part 2 Motions, or currents in the interior of a gas-giant planet such as Jupiter may be very different from the motions typical of the earth's interior. A second idea for the motions in the interior of a gas-giant As you move higher in the troposphere, the temperature drops, ranging from minus Fahrenheit minus Celsius to minus F minus C.

The next layer, the stratosphere, extends to almost miles km above the surface, containing hazes of hydrocarbons. Here, temperatures start at minus F and rise to approximately minus F minus C the higher you go.

The stratosphere, like the troposphere, is warmed by the sun and the planet's interior. The stratosphere ends where the pressure is one one-thousandth that found at the surface of Earth. The thermosphere lies on top of the stratosphere. Temperatures rise to approximately 1, F C at heights of over miles 1, km.

The aurora around the poles occurs within the thermosphere. The thermosphere can also emit a weak light known as airglow that keeps the night sky from ever being completely dark.

The thermosphere is heated by particles from the magnetosphere, as well as by the sun, and has no defined top. The outermost layer of Jupiter's atmosphere is the exosphere, where gas particles can escape into space. With no clear boundary, the exosphere bleeds into interstellar space. In addition to the red and white bands that make Jupiter visually stunning, the planet also boasts a prominent feature known as the Great Red Spot.

First identified in the s , the spot is actually a violent storm located just south of the planet's equator.