Venus Upper Clouds and the UV Absorber From MESSENGER/MASCS Observations

Simple item page
dc.contributor.authorPérez-Hoyos, Santiago
dc.contributor.authorSánchez‐Lavega, Agustin
dc.contributor.authorGarcía Muñoz, Antonio
dc.contributor.authorIrwin, Patrick G. J.
dc.contributor.authorPeralta, Javier
dc.contributor.authorHolsclaw, Gregory
dc.contributor.authorMcClintock, William
dc.contributor.authorSanz‐Requena, José Francisco
dc.date.accessioned2019-12-09T16:20:30Z
dc.date.available2019-12-09T16:20:30Z
dc.date.issued2018-01-05
dc.description©2018. American Geophysical Union.en
dc.description.abstractOne of the most intriguing, long‐standing questions regarding Venus's atmosphere is the origin and distribution of the unknown UV absorber, responsible for the absorption band detected at the near‐UV and blue range of Venus's spectrum. In this work, we use data collected by Mercury Atmospheric and Surface Composition Spectrometer (MASCS) spectrograph on board the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission during its second Venus flyby in June 2007 to address this issue. Spectra range from 0.3 μm to 1.5 μm including some gaseous H2O and CO2 bands, as well as part of the SO2 absorption band and the core of the UV absorption. We used the NEMESIS radiative transfer code and retrieval suite to investigate the vertical distribution of particles in the equatorial atmosphere and to retrieve the imaginary refractive indices of the UV absorber, assumed to be well mixed with Venus's small mode 1 particles. The results show a homogeneous equatorial atmosphere, with cloud tops (height for unity optical depth) at 75 ± 2 km above surface. The UV absorption is found to be centered at 0.34 ± 0.03 μm with a full width at half maximum of 0.14 ± 0.01 μm. Our values are compared with previous candidates for the UV aerosol absorber, among which disulfur oxide (S2O) and dioxide disulfur (S2O2) provide the best agreement with our results.en
dc.identifier.eissn2169-9100
dc.identifier.issn2169-9097
dc.identifier.urihttps://depositonce.tu-berlin.de/handle/11303/10460
dc.identifier.urihttp://dx.doi.org/10.14279/depositonce-9412
dc.language.isoenen
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subject.ddc550 Geowissenschaftende
dc.subject.othervenusen
dc.subject.otheratmospheresen
dc.subject.otherradiative transferen
dc.subject.otherspectroscopyen
dc.titleVenus Upper Clouds and the UV Absorber From MESSENGER/MASCS Observationsen
dc.typeArticleen
dc.type.versionpublishedVersionen
dcterms.bibliographicCitation.doi10.1002/2017JE005406en
dcterms.bibliographicCitation.issue1en
dcterms.bibliographicCitation.journaltitleJournal of Geophysical Research: Planetsen
dcterms.bibliographicCitation.originalpublishernameAmerican Geophysical Unionen
dcterms.bibliographicCitation.originalpublisherplaceHoboken, NJen
dcterms.bibliographicCitation.pageend162en
dcterms.bibliographicCitation.pagestart145en
dcterms.bibliographicCitation.volume123en
tub.accessrights.dnbdomainen
tub.affiliationFak. 2 Mathematik und Naturwissenschaften::Zentrum für Astronomie und Astrophysikde
tub.affiliation.facultyFak. 2 Mathematik und Naturwissenschaftende
tub.affiliation.instituteZentrum für Astronomie und Astrophysikde
tub.publisher.universityorinstitutionTechnische Universität Berlinen

Files

Original bundle
Now showing 1 - 1 of 1
Thumbnail Image
Name:
Perez-Hoyos_et_al-2018.pdf
Size:
2.11 MB
Format:
Adobe Portable Document Format
Description:
Published article
Download
License bundle
Now showing 1 - 1 of 1
No Thumbnail Available
Name:
license.txt
Size:
4.9 KB
Format:
Item-specific license agreed upon to submission
Description:
Download

Collections

Publications