Models of Venus Atmosphere

Lebonnois, Sébastien; Lee, Christopher; Yamamoto, Masaru; Dawson, Jonathan; Lewis, S. R.; Mendonça, João M.; Read, P. L.; Parish, H. F.; Schubert, G.; Bengtsson, Lennart; Grinspoon, David; Limaye, S. S.; Schmidt, Hauke; Svedhem, H.; Titov, D.

doi:10.1007/978-1-4614-5064-1_8

Cited by 32 publications

(45 citation statements)

References 24 publications

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“…If the residual error shown in Fig. 3 continue to grow, it would reach approximately 2% of total angular momentum after 1000 years, four times longer than a typical run in Lebonnois et al (2011) and more than 10 times longer than the time required to initialize a steady state from rest with the Lee et al (2007) configuration (95% of the AM is present after 96 years of simulation). Over the entire integration, physical torques (sp) apply an average of 2:344 Â 10 18 kg m 2 s À2 , compared to an actual rate of change ( @Mc @t ) of 2:357 Â 10 18 kg m 2 s À2 .…”

Section: Resultsmentioning

confidence: 91%

“…Lebonnois et al, 2011;Lee et al, 2007). Both suggested that the simplified forcing alone was insufficient to produce a realistic atmospheric state with their GCMs.…”

Section: Discussionmentioning

confidence: 93%

“…We have shown in an integration of the simplified FMS Venus GCM (Lee and Richardson, 2010) that angular momentum is conserved to a rate of better than 2% per 1000 years, with 98% of the angular momentum being directly attributable to the torques applied through the lower boundary layer. The longest integrations used in recent publications are the multi-century integrations in Lebonnois et al (2011) (the ''ISSI inter-comparison''), too short for numerical non-conservation to have a significant impact in the FMS Venus GCM. This result satisfies a fundamental requirement for GCMs that is necessary before more advanced physical forcing can meaningfully be examined in Venus models.…”

Section: Discussionmentioning

confidence: 99%

“…These GCMs are configured using the forcing described in Lee et al (2007) (referred to by the authors as the ''ISSI configuration'', Lebonnois et al (2011)) with a simple linear relaxation scheme to represent the radiative forcing of the atmosphere (c.f. Held and Suarez, 1994) and a Rayleigh friction boundary layer that relaxes the surface layer winds to rest over multi-day time-scales.…”

Section: Context For the Experimentsmentioning

confidence: 99%

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Angular momentum conservation in a simplified Venus General Circulation Model

Lee

Richardson²

2012

Icarus

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Section: Resultsmentioning

confidence: 91%

“…Lebonnois et al, 2011;Lee et al, 2007). Both suggested that the simplified forcing alone was insufficient to produce a realistic atmospheric state with their GCMs.…”

Section: Discussionmentioning

confidence: 93%

Section: Discussionmentioning

confidence: 99%

Section: Context For the Experimentsmentioning

confidence: 99%

See 2 more Smart Citations

Angular momentum conservation in a simplified Venus General Circulation Model

Lee

Richardson²

2012

Icarus

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“…Rossby waves are the obvious way to generate an upgradient transfer, and in a slowly rotating regime (such as Titan) they seem to be excited in conjunction with Kelvin waves, with a Doppler shift allowing phase locking, but by no means is the mechanism transparent [100,101]. Detailed GCMs still have trouble reproducing the zonal wind on Venus [102], and the mechanism of superrotation on the gas giants almost certainly differs again (e.g. [103,104])-even if the jets are shallow.…”

Section: (C) Planetary Atmospheresmentioning

confidence: 99%

Geophysical fluid dynamics: whence, whither and why?

Vallis¹

2016

Proc. R. Soc. A.

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A contribution to the special feature 'Perspectives in astrophysical and geophysical fluids' . GKV, This article discusses the role of geophysical fluid dynamics (GFD) in understanding the natural environment, and in particular the dynamics of atmospheres and oceans on Earth and elsewhere. GFD, as usually understood, is a branch of the geosciences that deals with fluid dynamics and that, by tradition, seeks to extract the bare essence of a phenomenon, omitting detail where possible. The geosciences in general deal with complex interacting systems and in some ways resemble condensed matter physics or aspects of biology, where we seek explanations of phenomena at a higher level than simply directly calculating the interactions of all the constituent parts. That is, we try to develop theories or make simple models of the behaviour of the system as a whole. However, these days in many geophysical systems of interest, we can also obtain information for how the system behaves by almost direct numerical simulation from the governing equations. The numerical model itself then explicitly predicts the emergent phenomenathe Gulf Stream, for example-something that is still usually impossible in biology or condensed matter physics. Such simulations, as manifested, for example, in complicated general circulation models, have in some ways been extremely successful and one may reasonably now ask whether understanding a complex geophysical system is necessary for predicting it. In what follows we discuss such issues and the roles that GFD has played in the past and will play in the future.

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General circulation driven by baroclinic forcing due to cloud layer heating: Significance of planetary rotation and polar eddy heat transport

Yamamoto

Takahashi

2016

JGR Planets

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A high significance of planetary rotation and poleward eddy heat fluxes is determined for general circulation driven by baroclinic forcing due to cloud layer heating. In a high-resolution simplified Venus general circulation model, a planetary-scale mixed Rossby-gravity wave with meridional winds across the poles produces strong poleward heat flux and indirect circulation. This strong poleward heat transport induces downward momentum transport of indirect cells in the regions of weak high-latitude jets. It also reduces the meridional temperature gradient and vertical shear of the high-latitude jets in accordance with the thermal wind relation below the cloud layer. In contrast, strong equatorial superrotation and midlatitude jets form in the cloud layer in the absence of polar indirect cells in an experiment involving Titan's rotation. Both the strong midlatitude jet and meridional temperature gradient are maintained in the situation that eddy horizontal heat fluxes are weak. The presence or absence of strong poleward eddy heat flux is one of the important factors determining the slow or fast superrotation state in the cloud layer through the downward angular momentum transport and the thermal wind relation. For fast Earth rotation, a weak global-scale Hadley circulation of the low-density upper atmosphere maintains equatorial superrotation and midlatitude jets above the cloud layer, whereas multiple meridional circulations suppress the zonal wind speed below the cloud layer.

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Models of Venus Atmosphere

Cited by 32 publications

References 24 publications

Angular momentum conservation in a simplified Venus General Circulation Model

Angular momentum conservation in a simplified Venus General Circulation Model

Geophysical fluid dynamics: whence, whither and why?

General circulation driven by baroclinic forcing due to cloud layer heating: Significance of planetary rotation and polar eddy heat transport

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