Radiative Energy Balance in the Venus Atmosphere

Titov, Dmitrij; Piccioni, G.; Drossart, P.; Markiewicz, W. J.

doi:10.1007/978-1-4614-5064-1_4

Cited by 13 publications

(11 citation statements)

References 72 publications

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“…The overall picture these provide of Venus's atmospheric energy budget have been reviewed in some detail e.g. by Titov et al () and discussed further in the context of a schematic energy budget by Schubert and Mitchell (). However, it is not clear how representative of the entire planet the measured fluxes are, since with a small number of probes (which typically can survive only a few hours at the high temperatures in the deep atmosphere) it is only feasible to sample a limited range of latitudes and times of the solar day.…”

Section: Venussupporting

confidence: 93%

“…However, it is not clear how representative of the entire planet the measured fluxes are, since with a small number of probes (which typically can survive only a few hours at the high temperatures in the deep atmosphere) it is only feasible to sample a limited range of latitudes and times of the solar day. Moreover, uncertainties in even the best directly measured radiative fluxes on Venus are generally quite large (Titov et al ), so the Venus energy budget is not very tightly constrained by observations.…”

Section: Venusmentioning

confidence: 99%

“…Although isolated examples of similar diagrams to those published for the Earth can be found for planets such as Venus (e.g. Taylor, ; Titov et al, ) and Mars (e.g. Read and Lewis, ; Taylor, ), these are typically incomplete and of doubtful accuracy in some cases, often relying on relatively crude estimates of key parameters.…”

Section: Introductionmentioning

confidence: 99%

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Global energy budgets and ‘Trenberth diagrams’ for the climates of terrestrial and gas giant planets

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Barstow

Charnay

et al. 2016

Quart J Royal Meteoro Soc

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The climate on Earth is generally determined by the amount and distribution of incoming solar radiation, which must be balanced in equilibrium by the emission of thermal radiation from the surface and atmosphere. The precise routes by which incoming energy is transferred from the surface and within the atmosphere and back out to space, however, are important features that characterize the current climate. This has been analyzed in the past by several groups over the years, based on combinations of numerical model simulations and direct observations of the Earth's climate system. The results are often presented in schematic form to show the main routes for the transfer of energy into, out of and within the climate system. Although relatively simple in concept, such diagrams convey a great deal of information about the climate system in a compact form. Such an approach has not so far been widely adopted in any systematic way for other planets of the Solar System, let alone beyond, although quite detailed climate models of several planets are now available, constrained by many new observations and measurements. Here we present an analysis of the global transfers of energy within the climate systems of a range of planets within the Solar System, including Mars, Titan, Venus and Jupiter, as modelled by relatively comprehensive radiative transfer and (in some cases) numerical circulation models. These results are presented in schematic form for comparison with the classical global energy budget analyses for the Earth, highlighting important similarities and differences. We also take the first steps towards extending this approach to other Solar System and extrasolar planets, including Mars, Venus, Titan, Jupiter and the 'hot Jupiter' exoplanet HD 189733b, presenting a synthesis of both previously published and new calculations for all of these planets.

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Section: Venussupporting

confidence: 93%

Section: Venusmentioning

confidence: 99%

See 1 more Smart Citation

Global energy budgets and ‘Trenberth diagrams’ for the climates of terrestrial and gas giant planets

Read

Barstow

Charnay

et al. 2016

Quart J Royal Meteoro Soc

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“…The atmospheric rotation period (6 to 8 days), radiative timescale (1 to 10 days; Crisp and Titov 1997;Titov et al 2013), and Venusian solar day (117 days) are longer than that of the microscale eddy timescale (a few hours). Atmospheric radiative and rotational processes are not included, because the heating rate of approximately 1 K · day −1 (approximately 0.04 K h −1 ) and the rotation rate are not significant for dynamical phenomena with timescales of a few hours.…”

Section: Model Assumptionsmentioning

confidence: 99%

Idealized numerical experiments on microscale eddies in the Venusian cloud layer

Yamamoto

2014

Earth Planet Sp

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Three-dimensional microscale dynamics of convective adjustment and mixing in and around the Venusian lower cloud layer were investigated using an idealized Weather Research and Forecasting (WRF) model. As control parameters of the idealized experiment, the present work introduces an initial lapse rate in the convective layer and thermal flux associated with the infrared flux gap at cloud base. Eddy heat, material, and momentum fluxes increase in the convective layer with the increase of these two parameters. In the case of convective adjustment over a very short period, prior to formation of a large-scale convective cell, transient microscale eddies efficiently and rapidly eliminate the convective instability. In the case of convective mixing induced by cloud-based thermal flux, microscale eddies are induced around a thin unstable layer at the cloud base, and spread to the middle and upper parts of the neutral layer. For atmospheric static stability around 55 km, two types of fine structure are found: a wave-like profile induced by weak microscale eddies, and a profile locally enhanced by strong eddies.

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“…A recent review of the radiative balance of Venus atmosphere can be found in Titov et al [, ]. Relevant observations to determine this energy balance are mostly obtained from orbit or from Earth: reflected solar radiation, observed albedo, thermal emission from the cloud top, and thermal emission from the lower atmosphere observed through near‐infrared windows.…”

Section: Introductionmentioning

confidence: 99%

Analysis of the radiative budget of the Venusian atmosphere based on infrared Net Exchange Rate formalism

Lebonnois

Eymet²,

Lee

et al. 2015

JGR Planets

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A detailed one-dimensional analysis of the energy balance in Venus atmosphere is proposed in this work, based on the Net Exchange Rate formalism that allows the identification in each altitude region of the dominant energy exchanges controlling the temperature. Well-known parameters that control the temperature profile are the solar flux deposition and the cloud particle distribution. Balance between solar heating and infrared energy exchanges is analyzed for each region: upper atmosphere (from cloud top to 100 km), upper cloud, middle cloud, cloud base, and deep atmosphere (cloud base to surface). The energy accumulated below the clouds is transferred to the cloud base through infrared windows, mostly at 3-4 μm and 5-7 μm. The continuum opacity in these spectral regions is not well known for the hot temperatures and large pressures of Venus's deep atmosphere but strongly affects the temperature profile from cloud base to surface. From cloud base, upward transport of energy goes through convection and short-range radiative exchanges up to the middle cloud where the atmosphere is thin enough in the 20-30 μm window to cool directly to space. Total opacity in this spectral window between the 15 μm CO 2 band and the CO 2 collision-induced absorption has a strong impact on the temperature in the cloud convective layer. Improving our knowledge of the gas opacities in these different windows through new laboratory measurements or ab initio computations, as well as improving the constraints on cloud opacities would help to separate gas and cloud contributions and secure a better understanding of Venus's atmosphere energy balance.

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Radiative Energy Balance in the Venus Atmosphere

Cited by 13 publications

References 72 publications

Global energy budgets and ‘Trenberth diagrams’ for the climates of terrestrial and gas giant planets

Global energy budgets and ‘Trenberth diagrams’ for the climates of terrestrial and gas giant planets

Idealized numerical experiments on microscale eddies in the Venusian cloud layer

Analysis of the radiative budget of the Venusian atmosphere based on infrared Net Exchange Rate formalism

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