Comparative analysis of airglow emissions in terrestrial planets, observed with VIRTIS-M instruments on board Rosetta and Venus Express

Migliorini, A.; Piccioni, G.; Capaccioni, F.; Filacchione, G.; Tosi, F.; Gérard, Jean‐Claude

doi:10.1016/j.icarus.2013.07.027

Cited by 11 publications

(10 citation statements)

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“…The instrument periodically measures internal background and dark current by closing an internal shutter, placed at the spectrometer's slit, and automatically subtracts it from the science data before transmitting data on ground. Once on the ground, the raw data are converted in spectral radiance by applying the calibration pipeline (Filacchione 2006;Ammannito et al 2006;Filacchione et al 2006) and additional corrections derived from in-fight data (Migliorini et al 2013;Raponi 2014). …”

Section: Virtis-m Descriptionmentioning

confidence: 99%

Water and carbon dioxide distribution in the 67P/Churyumov-Gerasimenko coma from VIRTIS-M infrared observations

Migliorini

Piccioni

Capaccioni

et al. 2016

A&A

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Context. Studying the coma environment of comet 67P/Churyumov-Gerasimenko (67P) is one of the primary scientific goals of the VIRTIS experiment on the ESA Rosetta mission. Aims. The distribution and variability of water vapour and carbon dioxide in the comet's coma are needed to estimate their production rate, abundances in the nucleus, and the spatial distribution of the active regions. Methods. Infrared emission lines from vibrational bands of water and carbon dioxide at 2.67 and 4.27 µm, respectively, were observed by the VIRTIS-M imaging channel and mapped from close to the nucleus up to ∼10 km altitude with a resolution of ∼40 m/px. A dataset consisting of 74 observations in the 1−5 µm spectral range acquired from 8 to 14 April 2015 when 67P was at a heliocentric distance of 1.9 AU is analysed in this work. A statistical correlation between the gas distribution and the surface's active regions was performed. Results. The maximum H 2 O emission is observed within 3 km from the nucleus and is mainly concentrated above two active regions, Aten-Babi and Seth-Hapi, while the CO 2 distribution appears more uniform with significant emissions coming from both the "head" and southern latitude regions. In the equatorial region, the column densities of both species decrease with altitude, although CO 2 decreases more rapidly than H 2 O. The calculated CO 2 /H 2 O column density ratios above Aten-Babi and Seth-Hapi are 2.4 ± 0.6% and 3.0 ± 0.7%, respectively. A value equal to 3.9 ± 1.0% is observed at equatorial latitudes in the region encompassing Imothep. Conclusions. VIRTIS-M has mapped the distribution of water vapour and carbon dioxide around the nucleus of 67P with unprecedented spatial resolution. The different water and carbon dioxide outgassing above the surface, seen in the VIRTIS-M data, might be indicative of a different thermal history of the northern and southern hemispheres of 67P.

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Section: Virtis-m Descriptionmentioning

confidence: 99%

Water and carbon dioxide distribution in the 67P/Churyumov-Gerasimenko coma from VIRTIS-M infrared observations

Migliorini

Piccioni

Capaccioni

et al. 2016

A&A

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“…The main scientific objectives of the Rosetta mission dealt with the study of the comet 67P/C‐G, with special emphasis on its nucleus and coma. Gravity assist maneuvers with the Earth and Mars [ Coradini et al ., ; Migliorini et al ., ] were performed during the 10 year long cruise phase, as well as flybys with the main belt asteroids (2867) Steins [ Tosi et al ., ; Leyrat et al ., ] and (21) Lutetia [ Coradini et al ., ]. The investigation of the planetary airglow emissions is one of the goals foreseen for the mission during the Earth and Mars flybys.…”

Section: Data Selectionmentioning

confidence: 99%

“…Since VIRTIS‐M spectral range extends up to 5.1 µm, thermal environment plays a major role in the instrumental performance. During the flyby, the VIRTIS radiator FOV was partially filled with the Earth, resulting in an optical bench temperature of about 147 K, significantly larger than the typical operative temperature of 135 K. This excess in temperature results in a wavelength shift of ~11 nm in the spectral calibration [ Migliorini et al ., ], which was corrected in the calibration pipeline [ Filacchione et al ., ].…”

Section: Data Selectionmentioning

confidence: 99%

“…A more detailed description of the Earth's observations with VIRTIS was given in Migliorini et al . [] and Hurley et al . [].…”

Section: Data Selectionmentioning

confidence: 99%

“…Finally, a spectral calibration adjustment has been performed by applying a shift of ~11 nm toward shorter wavelengths (see also Migliorini et al . []). The shaded area indicates the experimental error, calculated from the Noise Equivalent Spectral Radiance.…”

Section: Data Selectionmentioning

confidence: 99%

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Terrestrial OH nightglow measurements during the Rosetta flyby

Migliorini

Gérard

Soret

et al. 2015

Geophysical Research Letters

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We present a study of the terrestrial hydroxyl nightglow emissions observed with the Visible and Infrared Thermal Imaging Spectrometer on board the Rosetta mission. During these observations, the OH Δv = 1 and 2 sequences were measured simultaneously. This allowed investigating the relative population of the v = 1 to 9 vibrational levels by using both sequences. In particular, the relative population of the vibrational level v = 1 is determined for the first time from observations. The vibrational population decreases with increasing vibrational quantum number. A good agreement is found with a recent model calculation assuming multiquantum relaxation for OH(v) quenching by O2 and single‐quantum relaxation for OH(v) by N2.

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Aeronomy of the Venus Upper Atmosphere

et al. 2017

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We present aeronomical observations collected using remote sensing instruments on board Venus Express, complemented with ground-based observations and numerical modeling. They are mostly based on VIRTIS and SPICAV measurements of airglow obtained in the nadir mode and at the limb above 90 km. They complement our understanding of the behavior of Venus' upper atmosphere that was largely based on Pioneer Venus observations mostly performed over thirty years earlier. Following a summary of recent spectral data from the EUV to the infrared, we examine how these observations have improved our knowledge of the composition, thermal structure, dynamics and transport of the Venus upper atmosphere. We then synthesize progress in three-dimensional modeling of the upper atmosphere which is largely based on global mapping and observations of time variations of the nitric oxide and O 2 nightglow emissions. Processes controlling the escape flux of atoms to space are described. Results based on the VeRA radio propagation experiment are summarized and compared to ionospheric measurements collected during earlier space missions. Finally, we point out some unsolved and open questions generated by these recent datasets and model comparisons.

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Comparative analysis of airglow emissions in terrestrial planets, observed with VIRTIS-M instruments on board Rosetta and Venus Express

Cited by 11 publications

References 94 publications

Water and carbon dioxide distribution in the 67P/Churyumov-Gerasimenko coma from VIRTIS-M infrared observations

Water and carbon dioxide distribution in the 67P/Churyumov-Gerasimenko coma from VIRTIS-M infrared observations

Terrestrial OH nightglow measurements during the Rosetta flyby

Aeronomy of the Venus Upper Atmosphere

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