scholarly journals Dayside thermal structure of Venus' upper atmosphere characterized by a global model

2012 ◽  
Vol 117 (E8) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. S. Brecht ◽  
S. W. Bougher
Keyword(s):  
Thermal Structure ◽  
Global Model ◽  
Upper Atmosphere

The thermal structure and energy balance of the Uranian upper atmosphere

Icarus ◽  
1983 ◽  
Vol 53 (3) ◽  
pp. 399-414 ◽  
Author(s):  
R.G. French ◽  
J.L. Elliot ◽  
E.W. Dunham ◽  
D.A. Allen ◽  
J.H. Elias ◽  
...  
Keyword(s):  
Energy Balance ◽  
Thermal Structure ◽  
Upper Atmosphere

scholarly journals Observations of jupiter'S cloud structure near 8.5 μ

1971 ◽  
Vol 40 ◽  
pp. 359-362
Author(s):  
J. A. Westphal
Keyword(s):  
Brightness Temperature ◽  
Thermal Structure ◽  
Thermal Flux ◽  
Upper Atmosphere ◽  
Cloud Structure ◽  
Cloud Tops

Measurements of the distribution of thermal flux along polar and equatorial scans across Jupiter suggest that the increase in brightness temperature near 8.5 μ observed by Gillett et al. may be caused by flux coming from near the cloud tops. Other possible sources are discussed and observational tests suggested which should clarify the thermal structure of the upper atmosphere.

Impact of photochemical hazes on the thermal structure of exoplanet atmospheres

2020 ◽  
Author(s):  
Panayotis Lavvas ◽  
Anthony Arfaux
Keyword(s):  
Chemical Composition ◽  
Gas Phase ◽  
Thermal Structure ◽  
Temperature Inversion ◽  
Upper Atmosphere ◽  
Lower Atmosphere ◽  
Cloud Formation ◽  
Electromagnetic Spectrum ◽  
Heating Efficiency ◽  
The Impact

<p>Transit observations reveal that a significant population of the detected exoplanets has hazy atmospheres (Sing et al. 2016). Although the relative contribution of clouds and photochemical aerosols is not yet fully clarified, the impact of haze particles on the thermal structure could be significant, as such particles can efficiently scatter and absorb radiation over a large part of the electromagnetic spectrum. Particularly, photochemical aerosols are anticipated to be present at pressures lower than those of cloud formation. The transit observations of HD 189733 b indicate that the haze opacity responsible for the UV-Visible slope is located at pressures between 1μbar and 1 mbar. As such low pressures, the presence of hazes could allow for strong temperature inversions due to the low atmospheric density. We investigate here the implications of such hazes on the exoplanet atmospheric thermal structure.</p> <p>We simulate the atmospheric thermal structure using a 1D radiative-convective model. The model utilizes non-equilibrium chemical composition results (Lavvas et al. 2014) for the gas phase composition, and haze particle size distributions calculated from an aerosol microphysical growth model (Lavvas & Koskinen 2017, Lavvas et al. 2019). We do not yet consider the non-LTE effects for the gases, but we do take into account the impact of temperature disequilibrium between the particles and the gas envelope that can strongly affect the heating efficiency of the particles. We consider various gas phase opacities from atomic and molecular contributions calculated through correlated-k coefficients.</p> <p>Our results demonstrate that in the lower atmosphere the simulated temperature profiles provide emission spectra that are in good agreement with the eclipse observations for the simulated targets (HD 209458 b and HD 189733 b). In the upper atmosphere of the hazy HD 189733 b the simulated haze distribution, which fits the transit observations, results in a strong temperature inversion. On the contrary, the upper atmosphere of the clear HD 209458 b, is significantly colder compared to previous evaluations based on equilibrium chemistry assumption. The implications of these results on the chemical composition will be discussed, as well as results from other exoplanet cases.</p> <p> </p>

Thermal structure of Venus nightside upper atmosphere measured by stellar occultations with SPICAV/Venus Express

2015 ◽  
Vol 113-114 ◽  
pp. 321-335 ◽  
Author(s):  
A. Piccialli ◽  
F. Montmessin ◽  
D. Belyaev ◽  
A. Mahieux ◽  
A. Fedorova ◽  
...  
Keyword(s):  
Thermal Structure ◽  
Upper Atmosphere ◽  
Stellar Occultations ◽  
Venus Express

Titan's upper atmosphere: thermal structure, dynamics, and energetics

Titan ◽  
2014 ◽  
pp. 322-354
Author(s):  
R. V. Yelle ◽  
D. S. Snowden ◽  
I. C. F. Müller-Wodarg
Keyword(s):  
Thermal Structure ◽  
Upper Atmosphere ◽  
Structure Dynamics

The Temperature of the Upper Atmosphere*

1946 ◽  
Vol 27 (6) ◽  
pp. 331-342 ◽  
Author(s):  
R. Penndorf
Keyword(s):  
Sound Propagation ◽  
Thermal Structure ◽  
Upper Atmosphere ◽  
Atmospheric Tides ◽  
Polar Regions ◽  
Radiation Density ◽  
Direct Observations

Summary The thermal structure of the stratosphere and ionosphere is more elaborate than has heretofore been assumed. No appreciable rise in temperature up to 30 km is indicated from direct observations. A temperature of + 50°C at a height of 50 km is supported by the results on anomalous sound propagation, and of research on ozone and meteors, as well as by the theory of atmospheric tides. At heights around 50 to 80 km, the temperature again falls to −70°C, and afterwards rises again to somewhere between + 60°C and + 160°C at a height of 100 km. At heights around 200 to 250 km, the temperature is probably between + 160°C and + 560°C. In the polar regions at 100 km, the temperature is about −40°C, showing the marked difference due to latitude. A new definition for the concept of temperature in the upper atmosphere is given, since allowance must be made for radiation density.

scholarly journals Local Time Dependence of the Thermal Structure in the Venusian Equatorial Upper Atmosphere: Comparison of Akatsuki Radio Occultation Measurements and GCM Results

2018 ◽  
Vol 123 (9) ◽  
pp. 2270-2280 ◽  
Author(s):  
Hiroki Ando ◽  
Masahiro Takagi ◽  
Tetsuya Fukuhara ◽  
Takeshi Imamura ◽  
Norihiko Sugimoto ◽  
...  
Keyword(s):  
Time Dependence ◽  
Local Time ◽  
Radio Occultation ◽  
Thermal Structure ◽  
Upper Atmosphere ◽  
Local Time Dependence
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