Solar and thermal radiation in the Venus atmosphere

Moroz, V.I.; Ekonomov, A. P.; Moshkin, B. E.; Revercomb, H. E.; Sromovsky, Lawrence A.; Schofield, J. T.; Spänkuch, D.; Taylor, F. W.; Tomasko, M. G.

doi:10.1016/0273-1177(85)90202-9

Cited by 78 publications

(71 citation statements)

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“…solar heating that we calculated at 12-49 km is close to the values calculated by Moroz et al (1985). Figure 6 shows that the profile describing the atmospheric cooling due to the divergence of the infrared flux (skewed crosses) is close to the profile describing the atmospheric heating due to the divergence of solar and turbulent fluxes and dissipation of turbulent energy (crosses).…”

Section: (11)supporting

confidence: 55%

“…The profile of the planet-averaged solar flux is close to the profile measured by the Pioneer Venus large probe at a solar zenith angle of 66° (Tomasko et al , 1980;Moroz et al , 1985).…”

Section: Experimental Datamentioning

confidence: 93%

“…As there is no experimental data on temperature and wind pulsations for this zenith angle, we used the experimental profile of the solar-radiation flux from Moroz et al (1985) and the calculated flux of the atmospheric IR radiation from Marov et al (1985). At this solar zenith angle, as well as at smaller ones, the intensity of turbulence is higher than under average conditions, and normal turbulent convection extends throughout the entire troposphere.…”

Section: Introductionmentioning

confidence: 99%

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Turbulence in the troposphere of Venus: refined characteristics and new estimates

Izakov

2005

Sol Syst Res

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Based on spaceborne experimental data, characteristics of turbulence are calculated for the Venusian troposphere under conditions corresponding to the planet-averaged flux of solar radiation, which is equal to its value at a solar zenith angle of 66 ° . Additionally, given experimental data on radiation fluxes and their numerical calculations, turbulence characteristics were calculated for a solar zenith angle of 45 ° . The turbulence pattern is significantly different for small and large solar zenith angles. At large solar zenith angles, there exist an anomalous downward turbulent heat flux above 7-10 km and a normal upward flux at lower heights. At small zenith angles, the turbulent flux is normal throughout the entire troposphere. The dissipation of turbulent energy contributes significantly to the atmospheric heating in a wide range of altitudes. The spectrum of the time and space scales of dissipative processes in the troposphere is very wide and changes with height.

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Section: (11)supporting

confidence: 55%

“…The profile of the planet-averaged solar flux is close to the profile measured by the Pioneer Venus large probe at a solar zenith angle of 66° (Tomasko et al , 1980;Moroz et al , 1985).…”

Section: Experimental Datamentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

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Turbulence in the troposphere of Venus: refined characteristics and new estimates

Izakov

2005

Sol Syst Res

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“…The clouds, which result in a ~ 0.76 integrated-bond albedo for the planet (Moroz et al 1985), play a major role in controlling the energy balance of the atmosphere. Sulfuric acid cloud particles are produced through photochemistry near and above the cloud tops and through condensation in updrafts within the clouds (Krasnopolsky and Pollack 1994;Imamura and Hashimoto 2001); however, specific dynamical processes contributing to the transport of key species such as SO 2 and cloud droplets are unclear.…”

Section: Introductionmentioning

confidence: 99%

Overview of Akatsuki data products: definition of data levels, method and accuracy of geometric correction

Ogohara

Takagi

Murakami

et al. 2017

Earth Planets Space

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We provide an overview of data products from observations by the Japanese Venus Climate Orbiter, Akatsuki, and describe the definition and content of each data-processing level. Levels 1 and 2 consist of non-calibrated and calibrated radiance (or brightness temperature), respectively, as well as geometry information (e.g., illumination angles). Level 3 data are global-grid data in the regular longitude-latitude coordinate system, produced from the contents of Level 2. Non-negligible errors in navigational data and instrumental alignment can result in serious errors in the geometry calculations. Such errors cause mismapping of the data and lead to inconsistencies between radiances and illumination angles, along with errors in cloud-motion vectors. Thus, we carefully correct the boresight pointing of each camera by fitting an ellipse to the observed Venusian limb to provide improved longitude-latitude maps for Level 3 products, if possible. The accuracy of the pointing correction is also estimated statistically by simulating observed limb distributions. The results show that our algorithm successfully corrects instrumental pointing and will enable a variety of studies on the Venusian atmosphere using Akatsuki data.

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“…Soon after the rotation of Venus' atmosphere was discovered, Schubert and Whitehead (1969) suggested that superrotation could be produced by the slow motion of the subsolar point, a theory based on their laboratory results in which a moving bunsen flame heating a liquid could induce in it a mean flow. In the case of Venus, most of the sunlight absorption occurs between 45 and 70 km of altitude (Moroz et al, 1985), with the solar motion being eastwards and the atmosphere moving westwards. The waves thus excited will carry momentum away upwards and downwards from the region of excitation, consequently accelerating the fluid in the opposite direction the wave is moving, i.e.…”

Section: Introductionmentioning

confidence: 99%

Solar migrating atmospheric tides in the winds of the polar region of Venus

Peralta

Luz

Berry

et al. 2012

Icarus

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a b s t r a c tWe study the effects of migrating solar tides on the winds at the cloud tops of the polar region of Venus.The winds were measured using cloud tracking on images obtained at wavelengths of 3.9 and 5.0 lm by the instrument VIRTIS-M onboard Venus Express. These wavelengths probe about the same altitude close to the cloud tops, allowing for the first time to retrieve winds simultaneously in the day and nightside of the planet. We use a dataset with observations from 16 orbits, covering a time span of 289 days and a latitude range between 70°S and 85°S, the region where the so called cold collar resides. Diurnal and quarter-diurnal tides (wavenumbers 1 and 4) were detected in the wind field, with a decoupled influence on the zonal and meridional directions. The diurnal tide is the dominant harmonic with amplitudes of about 4.7 m/s exclusively affecting the meridional component of the wind and forcing a solar-to-antisolar circulation at the polar region. The quarter-diurnal mode is only apparent in the zonal wind in a restricted latitude range with amplitudes $2.2 m/s. The spatial structure of the diurnal tide has also been investigated, obtaining a vertical wavelength of about 8 km, in accordance with predictions by models. Finally, a theoretical relation between the amplitudes of tidal temperature and tidal wind has been derived and its validity tested with models and results from previous missions.

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Solar and thermal radiation in the Venus atmosphere

Cited by 78 publications

References 0 publications

Turbulence in the troposphere of Venus: refined characteristics and new estimates

Turbulence in the troposphere of Venus: refined characteristics and new estimates

Overview of Akatsuki data products: definition of data levels, method and accuracy of geometric correction

Solar migrating atmospheric tides in the winds of the polar region of Venus

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