Variable winds on Venus mapped in three dimensions

Sánchez‐Lavega, A.; Hueso, R.; Piccioni, G.; Drossart, P.; Peralta, Javier; Pérez‐Hoyos, S.; Wilson, Colin; Taylor, F. W.; Baines, K. H.; Luz, D.; Erard, S.; Lebonnois, Sébastien

doi:10.1029/2008gl033817

Cited by 126 publications

(156 citation statements)

References 16 publications

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“…For example Sánchez-Lavega et al (2008) found in Venus Express data that the zonal winds on Venus at the cloud level were approximately 60-100 m s −1 (the higher figure roughly at the tropopause level) from the equator out to about 5 50-60 • , and then decreased to the pole as is also seen here. They also found the peak meridional winds to be at 55 • S; this latitude is poleward of the Hadley cell on Earth.…”

supporting

confidence: 81%

Isca, v1.0: A Framework for the Global Modelling of the Atmospheres of Earth and Other Planets at Varying Levels of Complexity

Vallis¹,

Colyer²,

Geen³

et al. 2017

Preprint

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Abstract.Isca is a framework for the idealized modelling of the global circulation of planetary atmospheres at varying levels of complexity and realism. The framework is an outgrowth of models from the Geophysical Fluid Dynamics Laboratory designed for Earth's atmosphere, but it may readily be extended into other planetary regimes. Various forcing and radiation options are available, from dry, time invariant, Newtonian thermal relaxation to moist dynamics 5 with radiative transfer. Options are available in the dry thermal relaxation scheme to account for the effects of obliquity and eccentricity (and so seasonality), different atmospheric optical depths and a surface mixed layer. An idealized gray radiation scheme, a two-band scheme and a multi-band scheme are also available, all with simple moist effects and astronomically-based solar forcing. At the complex end of the spectrum the framework provides a direct connection to comprehensive atmospheric general circulation models. 10For Earth modeling, options include an aqua-planet and configurable continental outlines and topography.Continents may be defined by changing albedo, heat capacity and evaporative parameters, and/or by using a simple bucket hydrology model. Oceanic Q-fluxes may be added to reproduce specified sea-surface temperatures, with arbitrary continental distributions. Planetary atmospheres may be configured by changing planetary size and mass, solar forcing, atmospheric mass, radiative, and other parameters. Examples are given of various Earth configurations 15 as well as a Jovian simulation, a Venusian simulation, and tidally-locked and other orbitally-resonant exo-planet simulations.The underlying model is written in Fortran and may largely be configured with Python scripts. Python scripts are also used to run the model on different architectures, to archive the output, and for diagnostics, graphics, and post-processing. All of these features are publicly available on a git-based repository.

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supporting

confidence: 81%

Isca, v1.0: A Framework for the Global Modelling of the Atmospheres of Earth and Other Planets at Varying Levels of Complexity

Vallis¹,

Colyer²,

Geen³

et al. 2017

Preprint

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“…The westward wind speeds found in the 1-μm region are 65-75 m/s. This is slower than the nominal Super-Rotation speed of 100 m/s usually found in the UV imaging of the cloud top at around 65-72 km (Kawabata et al 1980;Limaye and Suomi 1981;Belton et al 1991;Peralta et al 2007;Sanchez-Lavega et al 2008;Ignatiev et al 2009;Hueso et al 2015). Some of the above concluded that the slower wind speed comes from the lower altitude sampled by the 1-µm images than in the UV region.…”

Section: Introductionmentioning

confidence: 76%

Initial products of Akatsuki 1-μm camera

Iwagami¹,

Sakanoi

Hashimoto

et al. 2018

Earth Planets Space

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The status and initial products of the 1-μm camera onboard the Akatsuki mission to Venus are presented. After the successful retrial of Venus' orbit insertion on Dec. 2015 (5 years after the failure in Dec. 2010), and after a long cruise under intense radiation, damage in the detector seems small and fortunately insignificant in the final quality of the images. More than 600 dayside images have been obtained since the beginning of regular operation on Apr. 2016 although nightside images are less numerous (about 150 in total at three wavelengths) due to the light scattered from the bright dayside. However, data acquisition stopped after December 07, 2016, due to malfunction of the electronics and has not been resumed since then. The 0.90-µm dayside images are of sufficient quality for the cloud-tracking procedure to retrieve wind field in the cloud region. The results appear to be similar to those reported by previous 1-μm imaging by Galileo and Venus Express. The representative altitude sampled for such dayside images is estimated to be 51-55 km. Also, the quality of the nightside 1.01-µm images is sufficient for a search for active volcanism, since interference due to cloud inhomogeneity appears to be insignificant. The quality of the 0.97-µm images may be insufficient to achieve the expected spatial resolution for the near-surface H 2 O mixing ratio retrievals.

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“…However, the limited local time coverage in these observations may allow a significant contamination of the thermal tide component, which can be up to ∼10 m s −1 (Newman and Leovy, 1992). At lower heights (∼50 km), cloud tracking using near-infrared wavelengths suggests a much weaker circulation, which is below the detection limit of these measurements of a few m s −1 (Belton et al, 1991;Sánchez-Lavega et al, 2008). The adiabatic heating of the high latitude stratosphere above the cloud, which is suggested by the temperature increase at high latitude (Crisp, 1989;Pätzold et al, 2007), and the increased CO mixing ratio in the high-latitude below the cloud layer (Collard et al, 1993;Tsang et al, 2008) are thought to be attributed to the downward branch of the cloud-level Hadley circulation.…”

Section: Meridional Circulationmentioning

confidence: 96%

Overview of Venus orbiter, Akatsuki

et al. 2011

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The Akatsuki spacecraft of Japan was launched on May 21, 2010. The spacecraft planned to enter a Venusencircling near-equatorial orbit in December 7, 2010; however, the Venus orbit insertion maneuver has failed, and at present the spacecraft is orbiting the Sun. There is a possibility of conducting an orbit insertion maneuver again several years later. The main goal of the mission is to understand the Venusian atmospheric dynamics and cloud physics, with the explorations of the ground surface and the interplanetary dust also being the themes. The angular motion of the spacecraft is roughly synchronized with the zonal flow near the cloud base for roughly 20 hours centered at the apoapsis. Seen from this portion of the orbit, cloud features below the spacecraft continue to be observed over 20 hours, and thus the precise determination of atmospheric motions is possible. The onboard science instruments sense multiple height levels of the atmosphere to model the three-dimensional structure and dynamics. The lower clouds, the lower atmosphere and the surface are imaged by utilizing nearinfrared windows. The cloud top structure is mapped by using scattered ultraviolet radiation and thermal infrared radiation. Lightning discharge is searched for by high speed sampling of lightning flashes. Night airglow is observed at visible wavelengths. Radio occultation complements the imaging observations principally by determining the vertical temperature structure.

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Variable winds on Venus mapped in three dimensions

Cited by 126 publications

References 16 publications

Isca, v1.0: A Framework for the Global Modelling of the Atmospheres of Earth and Other Planets at Varying Levels of Complexity

Isca, v1.0: A Framework for the Global Modelling of the Atmospheres of Earth and Other Planets at Varying Levels of Complexity

Initial products of Akatsuki 1-μm camera

Overview of Venus orbiter, Akatsuki

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