elib
DLR-Header
DLR-Logo -> http://www.dlr.de
DLR Portal Home | Impressum | Kontakt | English
Schriftgröße: [-] Text [+]

Venus surface and near surface anomalies on the Northern hemisphere observed by VIRTIS/VEX: First results

Arnold, Gabriele und Haus, Rainer und Kappel, David und Basilevsky, Alexander und Drossart, Pierre und Piccioni, Giuseppe (2009) Venus surface and near surface anomalies on the Northern hemisphere observed by VIRTIS/VEX: First results. In: Geophysical Research Abstracts, 11. EGU General Assembly 2009, 19.-24. Apr. 2010, Vienna, Austria.

[img]
Vorschau
PDF - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
121kB

Offizielle URL: http://meetingorganizer.copernicus.org/EGU2009/EGU2009-7878.pdf

Kurzfassung

Venus nightside emission measurements of VIRTIS on Venus Express provide the opportunity of surface studies in the narrow near infrared atmospheric windows. The measurements as well as detailed new radiative transfer simulations show that radiance ratios in the emission windows between 1.0 and 1.35 micron with respect to the 1.02 micron window can be used to extract information about the surface elevation and temperature. Based on these analyses, first surface and near surface anomalies are identified on the Northern hemisphere of Venus, which are due to deviations of the elevation - temperature correlation in certain small areas. The data are selected from VIRTIS-M-IR nightside measurements. To ensure minimal atmospheric influence on the measured signatures, only pushbroom observations with small observation angles close to nadir are taken into account. The radiative transfer simulation technique considers absorption, emission, and multiple scattering by gaseous and particulate constituents of the atmosphere. Look-up tables of quasi-monochromatic gas absorption cross-sections are calculated using appropriate spectral line data bases and line profiles and a line-by-line procedure. Empirical continuum absorption coefficients are determined from a ’VIRTIS reference spectrum’. In order to derive the parameters of the H2SO4 clouds, Mie theory is applied. Multiple scattering is considered by a Successive Order procedure. The synthetic quasi-monochromatic intensity spectra at the model top level of the atmosphere are convolved with the VIRTIS spectral response function. The surface windows at 1.02, 1.10 and 1.18 micron exhibit a clear dependence of transmitted radiation on topographical features and, thus, on surface thermal emission, since an elevation change of 12 km results in a temperature change of 100 K. In the first approximation, the radiance ratios are affine linear functions of the surface temperature. This is demonstrated by both measurements and simulations. In general, the ratio-based VIRTIS topography correlates well with the Magellan topography, but differences occur in localized areas. Different local surface anomalies do exist. These anomalies are probably a result of the lower atmosphere dynamics, errors in Magellan elevation determinations, or variations in the surface emissivity. Surface emissivity variations are important indicators of the nature of surface material. They may be due to variations in mineralogy and surface texture. While most of Venus’ geologic units are thought to be basaltic in composition, some of them (tessera terrains) could be felsic. The 1 micron emissivity of felsic materials is lower compared to basalts at similar texture conditions. Nevertheless, we found that anomalous areas comprise practically the same geologic units as adjacent non-anomalous terrains. The surface texture (grain size, packing density, surface roughness) is another important factor for emissivity anomalies. Grain size affects the spectral characteristics. Laboratory measurements of basalts and oxidized basalts show significant changes in the contrast of the 1 micron reflectivity band. Although most of the surface of Venus is not very rough, roughness variations exist. Tesserae and rifts show a higher surface roughness compared to other areas. Finally, the Magellan radar data that represent the base of the topography information of the Venus surface result from a surface layer of about 1 m in thickness, whereas the VIRTIS-NIR data describe the optical upper surface layer only. The radiative transfer simulations show the capability of our algorithm to investigate the surface of Venus. Based on these simulations and the VIRTIS/VEX measurements, the extracted anomalies are discussed in the framework of these processes and influences mentioned above. Future improvements will contribute to eliminate the masking of the Venus nightside windows by far wing and pressure-induced absorptions of the deep atmosphere constituents. This will allow a better separation of deep atmosphere, temperature, and emissivity contributions to the Venus nightside emission.

Dokumentart:Konferenzbeitrag (Vortrag)
Titel:Venus surface and near surface anomalies on the Northern hemisphere observed by VIRTIS/VEX: First results
Autoren:
AutorenInstitution oder E-Mail-Adresse der Autoren
Arnold, GabrieleGabriele.Arnold@dlr.de
Haus, RainerWestfälische Wilhelms-Universität Münster
Kappel, DavidWestfälische Wilhelms-Universität Münster
Basilevsky, AlexanderVernadsky Institute, Moscow, Russia
Drossart, PierreLESIA, Observatoire de Paris, France
Piccioni, GiuseppeINAF-IASF, Italy
Datum:23 April 2009
Erschienen in:Geophysical Research Abstracts
Referierte Publikation:Nein
In ISI Web of Science:Nein
Band:11
Status:veröffentlicht
Stichwörter:VIRTIS, VEX, Venus, retrieval, surface, anomalies
Veranstaltungstitel:EGU General Assembly 2009
Veranstaltungsort:Vienna, Austria
Veranstaltungsart:internationale Konferenz
Veranstaltungsdatum:19.-24. Apr. 2010
Veranstalter :European Geosciences Union
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W EW - Erforschung des Weltraums
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):W - Vorhaben Venus Express (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetenphysik
Hinterlegt von: David Kappel
Hinterlegt am:13 Jan 2011 14:19
Letzte Änderung:12 Dez 2013 21:13

Nur für Mitarbeiter des Archivs: Kontrollseite des Eintrags

Blättern
Suchen
Hilfe & Kontakt
Informationen
electronic library verwendet EPrints 3.3.12
Copyright © 2008-2013 Deutsches Zentrum für Luft- und Raumfahrt (DLR). Alle Rechte vorbehalten.