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dc.contributor.authorDias, J.A., Machado, P., Robert, S., Erwin, J., Lefèvre, M., Wilson, C.F., Quirino, D., Duarte, J.C.
dc.date2025
dc.date.accessioned2025-05-13T09:53:06Z
dc.date.available2025-05-13T09:53:06Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/14042
dc.descriptionVenus is home to thousands of volcanoes, with a wide range of volumes and sizes. Its surface is relatively young, with a temperature of approximately 735 K and an atmosphere of 92 bar. Past and possible ongoing volcanic outgassing is expected to provide a source to the sustenance of this massive atmosphere, dominated by CO2 and SO2. The lower atmosphere can be investigated in the near-infrared transparency windows on the nightside, such as the 2.3μm thermal emission window, which provides a chance of detection of species with volcanic origin, such as water vapor. The Planetary Spectrum Generator was used to simulate the nightside 2.3μm thermal emission window of Venus. We simulated the effect of a volcanic gas plume rising to a ceiling altitude, for species such as H2O, CO, OCS, HF and SO2. The sensitivity of the radiance spectrum at different wavelengths was explored as an attempt to qualitatively access detection for future measurements of both ground-based and space-instrumentation. We conclude from our qualitative analysis that for the H2O, CO and OCS plumes simulated there is potential to achieve a detection in the future, given a minimum required signal-to-noise ratio of 50. For SO2 and HF plumes, a higher signal-to-noise ratio would be needed.
dc.languageeng
dc.titleVolcanic gas plumes’ effect on the spectrum of Venus
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.subject.freeVenus
dc.subject.freeVolcano
dc.subject.freeWater plume
dc.subject.freeRadiative transfer
dc.subject.freeAtmosphere
dc.source.titleIcarus
dc.source.volume438
dc.source.pageA116589
Orfeo.peerreviewedYes
dc.identifier.doi10.1016/j.icarus.2025.116589
dc.identifier.url


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