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Isadore Silberman

, which only contribute to the atmosphere'smotion as rigid-body rotations relative to the earth,do not produce lateral stresses.6. Concluding remarksIn the preceding sections the harmonic tendencyequation has been derived, and it was shown how itmay be applied to the calculation of planetary flowpatterns. Although it is possible to carry out calculations for non-linear flow, it was shown in section fourthat the amount of computation is reduced greatly ifthe planetary waves are regarded as composed

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Takeshi Imamura, Yasuhiro Kawasaki, and Tetsuya Fukuhara

1. Introduction Atmospheric energy spectra as a function of horizontal wavenumber give clues as to the energy cycles of planetary atmospheres. The standard view for the terrestrial troposphere begins with the generation of zonal available potential energy by differential solar heating. This is converted to eddy available potential energy and eddy kinetic energy via baroclinic instability, principally in zonal wavenumbers 2–10 (e.g., Koshyk and Hamilton 2001 ). Nonlinear interactions transfer

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Michael J. Kavulich Jr., Istvan Szunyogh, Gyorgyi Gyarmati, and R. John Wilson

s = 60° takes 66.7 Sols, making the Northern Hemisphere winter significantly shorter than the Northern Hemisphere summer. In this paper, we refer to the time of the year by L s but describe the period and the frequency of the waves in Sols. c. The GFDL MGCM The GFDL MGCM has been used in a large number of studies of the Martian atmosphere. These studies have included investigations of tides and planetary waves ( Wilson and Hamilton 1996 ; Hinson and Wilson 2002 ; Wilson 2000 ; Hinson et al

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Daniel R. Chavas and Kevin A. Reed

scale (akin to a latitude-independent deformation radius) to the planetary radius. While both length scales are natural choices on dimensional grounds, they lack a direct connection to the dynamics of the atmosphere itself, particularly for the planetary radius. Moreover, these choices lack any dependence on latitude, which cannot be deduced solely from Buckingham Pi since such factors are themselves nondimensional. In our system, this parameter emerges as a ratio of two physical length scales

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N. G. Heavens

.1029/1999JE001095 . 10.1029/1999JE001095 Davy , R. , P. A. Taylor , W. Weng , and P.-Y. Li , 2009 : A model of dust in the Martian lower atmosphere . J. Geophys. Res. , 114 , D04108 , doi: 10.1029/2008JD010481 . Fenton , L. K. , and R. Lorenz , 2015 : Dust devil height and spacing with relation to the Martian planetary boundary layer thickness . Icarus , 260 , 246 – 262 , doi: 10.1016/j.icarus.2015.07.028 . 10.1016/j.icarus.2015.07.028 Forget , F. , and Coauthors , 1999

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William J. M. Seviour, Darryn W. Waugh, and Richard K. Scott

1. Introduction In common with several other planetary bodies, Mars’s atmosphere exhibits regions of strong circumpolar zonal winds known as polar vortices. These form in both the Northern and Southern Hemispheres during their respective winters and are an important barrier for the mixing of polar and midlatitude air. As such, they act to intensify meridional temperature gradients, influence the rate of condensation of CO 2 onto the polar ice cap, and limit the transport of dust and ice

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Junyan Xiong, Jun Yang, and Ji Nie

et al. 2016 ). The variation in atmospheric mass is common during the evolution of other planets. For instance, the persistent loss of Mars’s atmosphere has reduced its mass from 1 to 2 bar in its early stage to the present-day value of 0.006 bar ( Lammer and Bauer 1991 ). Atmospheric mass may play a key role in planetary habitability (e.g., Seager 2013 ). All of the above considerations inspire us to investigate the dependence of climate on atmospheric mass. Let us consider the possible

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Brian F. Farrell and Petros J. Ioannou

: Depth of a strong Jovian jet from a planetary-scale disturbance driven by storms. Nature , 451 , 437 – 440 . Scott , R. K. , and L. M. Polvani , 2007 : Forced-dissipative shallow-water turbulence on the sphere and the atmospheric circulation of the giant planets. J. Atmos. Sci. , 64 , 3158 – 3176 . Scott , R. K. , and L. M. Polvani , 2008 : Equatorial superrotation in shallow atmospheres. Geophys. Res. Lett. , 35 , L24202 . doi:10.1029/2008GL036060 . Sokolov , S. , and S

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Bingqiang Sun, George W. Kattawar, Ping Yang, and Eli Mlawer

.1175/1520-0469(1975)032<0409:TTSAIR>2.0.CO;2 . 10.1175/1520-0469(1975)032<0409:TTSAIR>2.0.CO;2 Coulson , K. L. , J. V. Dave , and Z. Sckera , 1960 : Tables Related to Radiation Emerging from a Planetary Atmosphere with Rayleigh Scattering . University of California Press, 548 pp. de Haan , J. F. , P. B. Bosma , and J. W. Hovenier , 1987 : The adding method for multiple scattering calculations of polarized light . Astron. Astrophys. , 183 , 371 – 391 . de Rooij , W. A. , 1985 : Reflection and transmission

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Nikolaos A. Bakas, Navid C. Constantinou, and Petros J. Ioannou

(2013a , 2014) addressed the emergence of the nonzonal coherent structures in barotropic beta-plane turbulence in terms of the parameters and , where β is the gradient of the planetary vorticity, is the length scale of the forcing, ε is the energy input rate of the forcing, and is the dissipation time scale. Characteristic values of these parameters for Earth’s midlatitude atmosphere and oceans and the Jovian atmosphere are given in Table 1 . It was found that for isotropic forcing the

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