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Kevin M. Grise and David W. J. Thompson

; Gettelman and Forster 2002 ; Fueglistaler et al. 2009 ). Zonal asymmetries in the TTL temperature field are predominantly linked to the quasi-stationary planetary wave pattern in the tropical troposphere ( Highwood and Hoskins 1998 ; Fueglistaler et al. 2009 ). These equatorial planetary waves reflect the equatorial Rossby and Kelvin wave responses to the climatological-mean distribution of latent heating from deep convection in the tropics ( Dima et al. 2005 ; Dima and Wallace 2007 ). The observed

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John Marshall and Damon W. K. So

15APmLI990 JOHN MARSHALL AND DAMON W. K. SO 963Thermal Equilibration of Planetary Waves JOHN MARSHALL AND DAMON W. K. SOSpace and Atmospheric Physics Group, Department of Physics, Imperial College, London, England(Manuscript received 28 October 1988, in final form 7 September 1989) ABSTRACT Equilibration of planetary waves toward free-mode forms, steady solutions of the unforced

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John R. Albers and Terrence R. Nathan

), photochemical damping of inertia–gravity waves ( Zhu and Holton 1986 ; Xu 1999 ; Xu et al. 2001 ), photochemical destabilization of free Rossby waves ( Nathan 1989 ; Nathan and Li 1991 ; Nathan et al. 1994 ), modulation of the quasi-biennial oscillation ( Cordero et al. 1998 ; Cordero and Nathan 2000 ), solar cycle modulation of both the quasi-biennial oscillation ( Cordero and Nathan 2005 ) and the Arctic polar vortex ( Nathan et al. 2011 ), and planetary wave drag ( Nathan and Cordero 2007

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Robert E. Dickinson

I969 R O 13 E R T E. D I C K I N S O N 73Theory of Planetary Wave-Zonal Flow Interaction ROBERT E. I)IClCINSON1 Massachusetts I~zstltute of Technology, Cambridge(Manuscript received 22 May 1968, in revised form 6 August 1968)ABSTRACT Small amplitude planetary waves are superimposed on a mean zonal flow with arbitrary horizontal andvertical shears. An expression is derived for the change of the zonal

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Isadore Silberman

coefficients as functions of all the harmonic coefficients. The harmonic tendencyequations may be used in an iterative process to find the flow pattern at a future time from a knowledge ofthe harmonic coefficients at an initial time.The amount of computation is reduced greatly if the planetary waves are regarded as composed of perturbations superimposed on a steady zonal flow in which the angular velocity varies with colatitude. Anexample based on an actual synoptic situation is given.The effect of large

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Anne K. Smith

two broad categories of forcing. The first is a planetary Rossby wave that propagates from below and therefore has a related structure in the stratosphere and mesosphere. The other is a planetary-scale variation in localized forcing of the mesospheric flow by gravity waves. There are several factors that could cause gravity wave driving to have large-scale asymmetries: gravity wave sources in the troposphere may be linked to fixed geographical features such as the continent/ocean distribution or

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Curt Covey and Gerald Schubert

NOVEMBER 1982CURT COVEY AND GERALD SCHUBERT2397Planetary-Scale Waves in the Venus AtmosphereCURT COVEYNational Center for Atmospheric Research1, Boulder, CO 80307GERALD SCHUBERTDepartment of Earth and Space Sciences, University of California, Los Angeles 90024(Manuscript received 10 May 1982, in final form 16 July 1982)ABSTRACTA numerical model of planetary-scale waves in Venus' atmosphere is used to simulate observed wave-likecloud features such as the dark horizontal Y. The model is based on

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Mark R. Schoeberl and John H. E. Clark

20 JOURNAL OF THE ATMOSPHERIC SCIENCES VOLUME 37Resonant Planetary Waves in a Spherical AtmosphereMARK R. SCHOEBERLNavul Research Laboratory, Washington, DC 20375JOHN H. E. CLARK'Science Application, Inc., McLean, VA 22102(Manuscript received 9 February 1979, in final form 21 August 1979) ABSTRACTIA global model of planetary wave propagation in a spherical atmosphere is used to examine thespectrum of free or resonant planetary waves of the solstitial stratosphere. These free

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Leo J. Donner and Hsiao-Lan Kuo

1 OCTOBER 1984 LEO J. DONNER AND HSIAO-LAN KUO 2849Radiative Forcing of Stationary Planetary Waves LEO J. DONNER National Center for Atmospheric Research, 1 Boulder, CO 80307 HSIAO-LAN KUO Department of the Geophysical Sciences, The University of Chicago, Chicago, IL 60637 (Manuscript received 9 January 1984, in final form 5 July 1984

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Carlos F. M. Raupp and Pedro L. Silva Dias

1. Introduction The atmospheric flow is characterized by the existence of low-frequency fluctuations with time scales ranging from 20 to around 100 days ( Madden and Julian 1972 , 1994 ; Hayashi and Golder 1993 ; Ghil and Mo 1991 ). The dominant component of this intraseasonal variability of the atmospheric circulation in the tropics is the 40–50-day Madden–Julian oscillation (MJO), which is characterized in the troposphere by a planetary-scale (wavenumber 1–2) wave envelope having an

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