H2N2V1, Main, Exploration, bibRecord, 002493

Titan: Far-infrared and microwave remote sensing of methane clouds and organic haze

Identifieur interne : 002493 ( Main/Exploration ); précédent : 002492; suivant : 002494

Titan: Far-infrared and microwave remote sensing of methane clouds and organic haze

Auteurs : W. Reid Thompson [États-Unis] ; Carl Sagan [États-Unis]

Source :

Icarus [ 0019-1035 ] ; 1984.

RBID : ISTEX:24C01C5D68A6C4E0E7B0188E4473D94DA9BF8DF2

English descriptors

Teeft :
- Absorption strength, Altitude, Altitude distribution, Arizona press, Astrophys, Atmospheric, Atmospheric gases, Atmospheric structure, Average voyager, Band shape, Birnbaum, Brightness temperature, Calculations show, Centimeter wavelengths, Cloud, Cloud altitudes, Cloud density, Cloud distribution, Cloud droplets, Cloud mass, Cloud material, Cloud opacity, Cloud particles, Column densities, Column density, Condensate, Condensed methane, Courtin, Emission angle, Emission angles, Emission spectra, Equal amounts, Error bars, Experimental data, Flasar, Further study, Hanel, Haze, Haze column density, Haze mass fraction, Haze opacity, Haze quantity, High altitude, Higher altitudes, Icarus, Infrared observations, Infrared spectrum, Iris, Irregular line, Jagged line, Khare, Kunde, Large array, Limb, Liquid absorption spectrum, Liquid methane, Liquid opacity, Little effect, Lower altitudes, Lower atmosphere, Lower frequencies, Lower limit, Mass fraction, Mesosphere, Mesospheric emission, Mesospheric emission models, Methane, Methane clouds, Microwave absorption, Millimeter wavelengths, Mole, Mole fraction, Mole fractions, Molecular mass, Numerical integration, Opacity, Opacity sources, Optical constants, Optical depth, Organic compounds, Organic haze, Overall slope, Overlying atmosphere, Particular interest, Phase absorption, Phys, Pure state, Quantitative determinations, Radiative, Sagan, Samuelson, Saturn system, Saturnian system, Smooth curves, Spectrum, Substantial land masses, Surface saturation, Surface temperature, Surface visibility, Temperature range, Thermal emission, Thermal emission properties, Thermal emission spectrum, Thermal opacity, Thermal radiation, Tholin, Titan, Titan atmosphere, Titan tholin, Titan tholin haze, Total column density, Total mass, Troposphere, Tropospheric, Upper atmosphere, Upper limit, Upper troposphere, Vapor pressure, Voyager, Voyager iris, Voyager observations, Wavelength.

Abstract

Abstract: It is shown that Titan's surface and plausible atmospheric thermal opacity sources—gaseous N2, CH4, and H2, CH4 cloud, and organic haze—are sufficient to match available Earth-based and Voyager observations of Titan's thermal emission spectrum. Dominant sources of thermal emission are the surface for wavelenghts λ ≳ 1 cm, atmospheric N2 for 1 cm ≳ λ ≳ 200 μm,, condensed and gaseous CH4 for 200 μm ≳ λ ≳ 20 μm, and molecular bands and organic haze for λ ≲ 20 μm. Matching computed spectra to the observed Voyager IRIS spectra at 7.3 and 52.7° emission angles yields the following abundances and locations of opacity sources: CH4 clouds: 0.1 g cm− at a planetocentric radius of 2610–2625 km, 0.3 g cm−2 at 2590–2610 km, total 0.4 ± 0.1 g cm–2 above 2590 km; organic haze: 4 ± 2 × 10−6, g cm, −2 above 2750 km; tropospheric H2: 0.3 ± 0.1 mol%. This is the first quantitative estimate of the column density of condensed methane (or CH4/C2H6) on Titan. Maximum transparency in the middle to far IR occurs at 19 μm where the atmospheric vertical absorption optical depth is ⋍0.6 A particle radius r ≲ 2 μm in the upper portion of the CH4 cloud is indicated by the apparent absence of scattering effects.

Url:

https://api.istex.fr/ark:/67375/6H6-40SBK0KR-5/fulltext.pdf

DOI: 10.1016/0019-1035(84)90187-8

Affiliations:

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Le document en format XML

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<term>Altitude</term>
<term>Altitude distribution</term>
<term>Arizona press</term>
<term>Astrophys</term>
<term>Atmospheric</term>
<term>Atmospheric gases</term>
<term>Atmospheric structure</term>
<term>Average voyager</term>
<term>Band shape</term>
<term>Birnbaum</term>
<term>Brightness temperature</term>
<term>Calculations show</term>
<term>Centimeter wavelengths</term>
<term>Cloud</term>
<term>Cloud altitudes</term>
<term>Cloud density</term>
<term>Cloud distribution</term>
<term>Cloud droplets</term>
<term>Cloud mass</term>
<term>Cloud material</term>
<term>Cloud opacity</term>
<term>Cloud particles</term>
<term>Column densities</term>
<term>Column density</term>
<term>Condensate</term>
<term>Condensed methane</term>
<term>Courtin</term>
<term>Emission angle</term>
<term>Emission angles</term>
<term>Emission spectra</term>
<term>Equal amounts</term>
<term>Error bars</term>
<term>Experimental data</term>
<term>Flasar</term>
<term>Further study</term>
<term>Hanel</term>
<term>Haze</term>
<term>Haze column density</term>
<term>Haze mass fraction</term>
<term>Haze opacity</term>
<term>Haze quantity</term>
<term>High altitude</term>
<term>Higher altitudes</term>
<term>Icarus</term>
<term>Infrared observations</term>
<term>Infrared spectrum</term>
<term>Iris</term>
<term>Irregular line</term>
<term>Jagged line</term>
<term>Khare</term>
<term>Kunde</term>
<term>Large array</term>
<term>Limb</term>
<term>Liquid absorption spectrum</term>
<term>Liquid methane</term>
<term>Liquid opacity</term>
<term>Little effect</term>
<term>Lower altitudes</term>
<term>Lower atmosphere</term>
<term>Lower frequencies</term>
<term>Lower limit</term>
<term>Mass fraction</term>
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<term>Mesospheric emission</term>
<term>Mesospheric emission models</term>
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<term>Methane clouds</term>
<term>Microwave absorption</term>
<term>Millimeter wavelengths</term>
<term>Mole</term>
<term>Mole fraction</term>
<term>Mole fractions</term>
<term>Molecular mass</term>
<term>Numerical integration</term>
<term>Opacity</term>
<term>Opacity sources</term>
<term>Optical constants</term>
<term>Optical depth</term>
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<term>Particular interest</term>
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<term>Phys</term>
<term>Pure state</term>
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<term>Sagan</term>
<term>Samuelson</term>
<term>Saturn system</term>
<term>Saturnian system</term>
<term>Smooth curves</term>
<term>Spectrum</term>
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<term>Surface saturation</term>
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<term>Surface visibility</term>
<term>Temperature range</term>
<term>Thermal emission</term>
<term>Thermal emission properties</term>
<term>Thermal emission spectrum</term>
<term>Thermal opacity</term>
<term>Thermal radiation</term>
<term>Tholin</term>
<term>Titan</term>
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<term>Titan tholin</term>
<term>Titan tholin haze</term>
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<term>Total mass</term>
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<term>Tropospheric</term>
<term>Upper atmosphere</term>
<term>Upper limit</term>
<term>Upper troposphere</term>
<term>Vapor pressure</term>
<term>Voyager</term>
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<term>Voyager observations</term>
<term>Wavelength</term>
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<front><div type="abstract" xml:lang="en">Abstract: It is shown that Titan's surface and plausible atmospheric thermal opacity sources—gaseous N2, CH4, and H2, CH4 cloud, and organic haze—are sufficient to match available Earth-based and Voyager observations of Titan's thermal emission spectrum. Dominant sources of thermal emission are the surface for wavelenghts λ ≳ 1 cm, atmospheric N2 for 1 cm ≳ λ ≳ 200 μm,, condensed and gaseous CH4 for 200 μm ≳ λ ≳ 20 μm, and molecular bands and organic haze for λ ≲ 20 μm. Matching computed spectra to the observed Voyager IRIS spectra at 7.3 and 52.7° emission angles yields the following abundances and locations of opacity sources: CH4 clouds: 0.1 g cm− at a planetocentric radius of 2610–2625 km, 0.3 g cm−2 at 2590–2610 km, total 0.4 ± 0.1 g cm–2 above 2590 km; organic haze: 4 ± 2 × 10−6, g cm, −2 above 2750 km; tropospheric H2: 0.3 ± 0.1 mol%. This is the first quantitative estimate of the column density of condensed methane (or CH4/C2H6) on Titan. Maximum transparency in the middle to far IR occurs at 19 μm where the atmospheric vertical absorption optical depth is ⋍0.6 A particle radius r ≲ 2 μm in the upper portion of the CH4 cloud is indicated by the apparent absence of scattering effects.</div>
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Titan: Far-infrared and microwave remote sensing of methane clouds and organic haze

Titan: Far-infrared and microwave remote sensing of methane clouds and organic haze

Source :

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri