EUV spectroscopy of the Venus dayglow with UVIS on Cassini

Gérard, Jean‐Claude; Hubert, Benoît; Gustin, Jacques; Shematovich, V. I.; Bisikalo, D. V.; Gladstone, G. Randall; Esposito, L. W.

doi:10.1016/j.icarus.2010.09.020

Cited by 48 publications

(28 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…5,6 Emissions originating from the B 1 S + (y ¼ 0), B 1 S + (y ¼ 1), and C 1 S + (y ¼ 0) vibrational levels were recorded from the Martian and Venusian atmospheres by the Hopkins Ultraviolet Telescope, 7 the FUSE satellite, 8,9 and the Cassini UVIS instrument. 10 Large CO abundances produce detectable signals even for the rare isotopologues, including 12 …”

Section: Introductionmentioning

confidence: 99%

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels

et al. 2016

View full text Add to dashboard Cite

show abstract

Section: Introductionmentioning

confidence: 99%

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels

et al. 2016

View full text Add to dashboard Cite

show abstract

“…Gérard et al . [] modeled the radiative transfer of the OI‐98.9 nm emission in the thermosphere of Venus, including photochemical sources and resonance scattering of solar photons. Their results compared well with the Cassini Ultraviolet Imaging Spectrograph (UVIS) EUV observation of the Venus thermosphere performed during the Cassini flyby of Venus, up to ~20% over the whole flyby with a much better accuracy over the portion of the flyby presenting the largest 98.9 nm intensity.…”

Section: Introductionmentioning

confidence: 99%

Nonthermal radiative transfer of oxygen 98.9 nm ultraviolet emission: Solving an old mystery

et al. 2015

Self Cite

View full text Add to dashboard Cite

Sounding rocket measurements conducted in 1988 under high solar activity conditions revealed that the intensity of thermospheric OI emissions at 98.9 nm presents an anomalous vertical profile, showing exospheric intensities much higher than expected from radiative transfer model results, which included the known sources of excited oxygen. All attempts based on modeling of the photochemical processes and radiative transfer were unable to account for the higher than predicted brightnesses. More recently, the SOHO‐Solar Ultraviolet Measurements of Emitted Radiation instrument measured the UV solar flux at high‐spectral resolution, revealing the importance of a significant additional source of oxygen emission at 98.9 nm that had not been accounted for before. In this study, we simulate the radiative transfer of the OI‐98.9 nm multiplet, including the photochemical sources of excited oxygen, the resonant scattering of solar photons, and the effects of nonthermal atoms, i.e., a population of fast‐moving oxygen atoms in excess of the Maxwellian distribution. Including resonance scattering of the 98.9 nm solar multiplet, we find good agreement with the previous sounding rocket observation. The inclusion of a nonthermal oxygen population with a consistent increase of the total density produces a larger intensity at high altitude that apparently better accounts for the observation, but such a correction cannot be demonstrated given the uncertainties of the observations. A good agreement between model and sounding rocket observation is also found with the triplet at 130.4 nm. We further investigate the radiative transfer of the OI‐98.9 nm multiplet and the oxygen emissions at 130.4 and 135.6 nm using observations from the STP78‐1 satellite. We find a less satisfying agreement between the model and the STP78‐1 data that can be accounted for by scaling the modeled intensity within a range acceptable given the uncertainties on the STP78‐1 absolute calibration.

show abstract

“…It is partly supplied by the capture of solar wind He ++ ions and surface outgassing (Krasnopolsky and Gladstone 2005;Chanteur et al 2009). In addition, emission lines from atomic carbon and nitrogen have also been finally observed on Mars and Venus (Feldman et al 2000;Krasnopolsky 2002;Gérard et al 2011). …”

Section: Compositionmentioning

confidence: 95%

“…More recently the Martian hydrogen corona has been observed by the UV spectrometer SPICAM ) on Mars Express, by the ALICE instrument on Rosetta during its flyby in February 2007 (Feldman et al 2011) and from Earth by FUSE (Feldman et al 2000) and the Hubble Space Telescope (Clarke et al 2009). The Venus hydrogen corona has been observed by the UV instruments SPICAV (Bertaux et al 2007) on Venus Express and UVIS on Cassini during its fly-by of Venus (Gérard et al 2011). In this section, we focus on the recent observations performed by the SPICAM-UV and SPICAV-UV instruments.…”

Section: Recent Observations Of Hydrogen Coronae By Uv Remote Sensingmentioning

confidence: 99%

“…H Lyman-α observations at higher altitudes need to be carefully corrected from the interplanetary emission component, which contributes to more than 70% of the signal above 10,000 km. Hydrogen observations by UVIS on Cassini during its Venus fly-by have been reported by Gérard et al (2011) but no detailed study has been performed yet. Hydrogen density profiles derived from published SPICAM-UV (one population model) and SPICAV-UV (near noon; Chaufray et al 2008Chaufray et al , 2011 are displayed on Fig.…”

Section: Recent Observations Of Hydrogen Coronae By Uv Remote Sensingmentioning

confidence: 99%

See 1 more Smart Citation

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

et al. 2011

View full text Add to dashboard Cite

International audienceOur understanding of the upper atmosphere of unmagnetized bodies such as Mars, Venus and Titan has improved significantly in this decade. Recent observations by in situ and remote sensing instruments on board Mars Express, Venus Express and Cassini have revealed characteristics of the neutral upper atmospheres (exospheres) and of energetic neutral atoms (ENAs). The ENA environment in the vicinity of the bodies is by itself a significant study field, but ENAs are also used as a diagnostic tool for the exosphere and the interaction with the upstream plasmas. Synergy between theoretical and modeling work has also improved considerably. In this review, we summarize the recent progress of our understanding of the neutral environment in the vicinity of unmagnetized planets

show abstract

EUV spectroscopy of the Venus dayglow with UVIS on Cassini

Cited by 48 publications

References 48 publications

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels

Nonthermal radiative transfer of oxygen 98.9 nm ultraviolet emission: Solving an old mystery

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

Contact Info

Product

Resources

About

EUV spectroscopy of the Venus dayglow with UVIS on Cassini

Cited by 48 publications

References 48 publications

VIS and VUV spectroscopy of 12C17O and deperturbation analysis of the A1Π, υ = 1–5 levels

VIS and VUV spectroscopy of 12C17O and deperturbation analysis of the A1Π, υ = 1–5 levels

Nonthermal radiative transfer of oxygen 98.9 nm ultraviolet emission: Solving an old mystery

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

Contact Info

Product

Resources

About

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels

VIS and VUV spectroscopy of ¹²C¹⁷O and deperturbation analysis of the A¹Π, υ = 1–5 levels