Search Results

You are looking at 51 - 60 of 16,860 items for :

  • Planetary atmospheres x
  • All content x
Clear All
Aiko Voigt, Isaac M. Held, and Jochem Marotzke

topic of atmospheric dynamics (e.g., Lorenz 1967 ; Schneider 2006 ). While geophysical fluid dynamics provides the underlying equations, the challenge in constructing Hadley cell theories is to identify which terms of these equations govern the Hadley cell under investigation, and which terms can be neglected. The long-term goal is a complete Hadley cell theory that is applicable to a wide range of climates and planetary atmospheres and incorporates the effect of latent heat release. It is

Full access
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

Full access
Junjun Liu and Tapio Schneider

relaxation times are measured in centuries and millennia, while at the same time resolving the energy-containing eddies in the upper atmospheres. Therefore, we focus on flows in the upper atmospheres, using a GCM that solves the hydrostatic primitive equations for a dry ideal-gas atmosphere in a thin spherical shell. The model is essentially that introduced for Jupiter in SL09 , but here we use it also to simulate Saturn, Uranus, and Neptune. 2 Parameters such as the planetary rotation rate

Full access
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

Full access
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

Full access
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

Full access
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

Full access
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

Full access
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

Restricted access
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

Full access