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Retrieval of surface emissivity from VIRTIS/VEX radiation measurements over the Northern hemisphere of Venus

Haus, Rainer and Arnold, Gabriele and Kappel, David (2010) Retrieval of surface emissivity from VIRTIS/VEX radiation measurements over the Northern hemisphere of Venus. In: Geophysical Research Abstracts, 12. EGU General Assembly 2010, 02.-07. May. 2010, Vienna, Austria.


Official URL: http://meetingorganizer.copernicus.org/EGU2010/EGU2010-2646.pdf


The radiation measurements of VIRTIS-M-IR (1-5 micron) on Venus Express provide a valuable database for systematic studies of the atmosphere and surface of Venus. The high variability of nightside atmospheric and surface emission window radiances with respect to cloud opacity and surface elevation is modeled and discussed in comparison with measurements performed over the Northern hemisphere. The radiative transfer simulations for a quantitative evaluation of atmospheric and surface parameters use the DISORT code and include absorption, emission, and multiple scattering by atmospheric gaseous and particulate constituents. Look-up tables of quasi-monochromatic absorption cross-sections of gaseous constituents are calculated on the basis of a line-by-line procedure that makes use of appropriate spectral line databases. Microphysical parameters of the four-mode H2SO4 clouds are calculated from Mie theory. Deep atmospheric window continuum absorption is estimated from simultaneous retrievals of many spectra that were recorded for a high variety of atmospheric and surface conditions. Due to the conservative scattering behavior of the clouds below 1.5 micron, radiance ratios of the emission windows, which are located between 1.10 and 1.35 micron, and the most topography sensitive window at 1.02 micron may serve to de-cloud the measurement data and yield a quick-look tool to extract the surface elevation. While the ratio-based VIRTIS topography is in good agreement with Magellan topography for most swaths, some differences occur in localized areas. Possible origins of such anomalies are discussed. They can be due to local surface or near surface temperature fluctuations, local unstable atmospheric dynamics, or still unknown spectral cloud features. Some of the predicted anomaly candidates were found to originate from measurement or calibration uncertainties, but some other point to variations of surface emissivity. Such variations are due to changes in the chemical composition (mineralogy) and/or surface texture. They are therefore important indicators of the nature of the surface material. Radiance retrievals along a number of complete Northern orbits reveal systematic trends towards lower values of highland surface emissivity compared with surrounding lowlands. This result is in accordance with increased Magellan radar reflectivities at high altitudes and supports the hypothesis of older highland regions with felsic rock components.

Item URL in elib:https://elib.dlr.de/68399/
Document Type:Conference or Workshop Item (Speech)
Title:Retrieval of surface emissivity from VIRTIS/VEX radiation measurements over the Northern hemisphere of Venus
AuthorsInstitution or Email of AuthorsAuthors ORCID iD
Haus, RainerWestfälische Wilhelms-Universität MünsterUNSPECIFIED
Arnold, GabrieleGabriele.Arnold (at) dlr.deUNSPECIFIED
Kappel, DavidWestfälische Wilhelms-Universität MünsterUNSPECIFIED
Date:5 May 2010
Journal or Publication Title:Geophysical Research Abstracts
Refereed publication:No
Open Access:Yes
Gold Open Access:No
In ISI Web of Science:No
Keywords:VIRTIS, VEX, Venus, retrieval, surface
Event Title:EGU General Assembly 2010
Event Location:Vienna, Austria
Event Type:international Conference
Event Dates:02.-07. May. 2010
Organizer:European Geosciences Union
HGF - Research field:Aeronautics, Space and Transport (old)
HGF - Program:Space (old)
HGF - Program Themes:W EW - Erforschung des Weltraums
DLR - Research area:Space
DLR - Program:W EW - Erforschung des Weltraums
DLR - Research theme (Project):W - Vorhaben Venus Express (old)
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Physics
Deposited By: Kappel, David
Deposited On:13 Jan 2011 14:18
Last Modified:31 Jul 2019 19:31

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