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Image of Jupiter's Great Red Spot from Voyager 1

Image of Jupiter's Great Red Spot, obtained during the fly-by of Jupiter by NASA's Voyager 1 spacecraft in 1979.

Credit: NASA/JPL

Prof. Peter Read

Emeritus/researcher

Research theme

  • Climate physics
  • Exoplanets and planetary physics

Sub department

  • Atmospheric, Oceanic and Planetary Physics

Research groups

  • Geophysical and Astrophysical Fluid Dynamics
  • Planetary Climate Dynamics
Peter.Read@physics.ox.ac.uk
Telephone: 01865 (2)72082
Atmospheric Physics Clarendon Laboratory, room 210
  • About
  • Publications

Generation of inertia-gravity waves in the rotating thermal annulus by a localised boundary layer instability

Geophys. Astrophys. Fluid Dyn. Taylor & Francis Ltd 105:2-3 (2011) 161-181

Authors:

TNL Jacoby, PL Read, PD Williams, RMB Young

Abstract:

Waves with periods shorter than the inertial period exist in the atmosphere (as inertia-gravity waves) and in the oceans (as Poincare and internal gravity waves). Such waves owe their origin to various mechanisms, but of particular interest are those arising either from local secondary instabilities or spontaneous emission due to loss of balance. These phenomena have been studied in the laboratory, both in the mechanically-forced and the thermally-forced rotating annulus. Their generation mechanisms, especially in the latter system, have not yet been fully understood, however. Here we examine short period waves in a numerical model of the rotating thermal annulus, and show how the results are consistent with those from earlier laboratory experiments. We then show how these waves are consistent with being inertia-gravity waves generated by a localised instability within the thermal boundary layer, the location of which is determined by regions of strong shear and downwelling at certain points within a large-scale baroclinic wave flow. The resulting instability launches small-scale inertia-gravity waves into the geostrophic interior of the flow. Their behaviour is captured in fully nonlinear numerical simulations in a finite-difference, 3D Boussinesq Navier-Stokes model. Such a mechanism has many similarities with those responsible for launching small- and meso-scale inertia-gravity waves in the atmosphere from fronts and local convection.
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THE MARTIAN ATMOSPHERIC BOUNDARY LAYER

REVIEWS OF GEOPHYSICS 49 (2011) ARTN RG3005

Authors:

A Petrosyan, B Galperin, SE Larsen, SR Lewis, A Maeaettaenen, PL Read, N Renno, LPHT Rogberg, H Savijarvi, T Siili, A Spiga, A Toigo, L Vazquez
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Thermal Structure and Dynamics of Saturn's Northern Springtime Disturbance

Science (2011) 1-5

Authors:

LN Fletcher, BE Hesman, PGJ Irwin, KH Baines, TW Momary, A Sanchez-Lavega, F Michael Flasar, PL Read, GS Orton, A Simon-Miller, R Hueso, GL Bjoraker, A Mamoutkine, T Del Rio-Gaztelurrutia, JM Gomez, B Buratti, RN Clark, PD Nicholson, C Sotin

Evidence for Climate Change on Mars

Chapter in Solar System Update, Springer (2010) 135

Authors:

SR Lewis, PL Read

Abstract:

This book, the first in a series of forthcoming volumes, consists of topical and timely reviews of a number of carefully selected topics in solar systemn science.
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Synchronization in a pair of thermally coupled rotating baroclinic annuli: understanding atmospheric teleconnections in the laboratory.

Phys Rev Lett 104:20 (2010) 204501

Authors:

AA Castrejón-Pita, PL Read

Abstract:

Synchronization phenomena in a fluid dynamical analogue of atmospheric circulation is studied experimentally by investigating the dynamics of a pair of thermally coupled, rotating baroclinic annulus systems. The coupling between the systems is in the well-known master-slave configuration in both periodic and chaotic regimes. Synchronization tools such as phase dynamics analysis are used to study the dynamics of the coupled system and demonstrate phase synchronization and imperfect phase synchronization, depending upon the coupling strength and parameter mismatch.
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