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Ground‐based near‐infrared observations of the Venus nightside: The thermal structure and water abundance near the surface
Abstract
We used ground‐based near‐infrared (NIR) observations of thermal emission from the Venus nightside to determine the temperature structure and water vapor distribution between the surface and the 6‐km level. We show that emission from spectral windows near 1.0, 1.1, and 1.18 μm originates primarily from the surface and lowest scale height (∼16 km). These windows include absorption by weak H 2 O and CO 2 lines and by the far wings of lines in strong nearby CO 2 bands. Rayleigh scattering by the 90‐bar CO 2 atmosphere and Mie scattering by the H 2 SO 4 clouds attenuate this emission, but add little to its spectral dependence. Surface topography also modulates this NIR thermal emission because high‐elevation regions are substantially cooler and emit less thermal radiation than the surrounding plains. These contributions to the emission are clearly resolved in moderate‐resolution (λ/Δλ ∼ 400) spectral image cubes of the Venus nightside acquired with the infrared imaging spectrometer (IRIS) on the Anglo‐Australian Telescope (AAT) in 1991. To analyze these observations, we used a radiative transfer model that includes all of the radiative processes listed above. Synthetic spectra for several topographic elevations were combined with Pioneer Venus altimetry data to generate spatially resolved maps of the NIR thermal emission. Comparisons between these synthetic radiance maps and the IRIS observations indicate no near‐infrared signature of the surface emissivity differences seen at microwave wavelengths by the Magellan orbiter. Assuming constant surface emissivity in the near‐infrared, we derive nightside averaged temperature lapse rates of −7 to −7.5 K/km in the lowest 6 km. These lapse rates are smaller and indicate much greater static stability than those inferred from earlier measurements and greenhouse models (−8 to −8.5 K/km) [ Seiff , 1983]. An acceptable fit to the data was obtained with an H 2 O mixing ratio profile which increases from 20 ppmv at the cloud base to 45 ppmv at 30 km, and then remains constant between that altitude and the surface. There is no evidence for H 2 O mixing ratios that decrease with altitude, like those inferred from the Pioneer Venus large probe mass spectrometer [ Donahue and Hodges , 1992a] or the Venera 11 and 12 Lander spectrophotometers [ Moroz , 1983].
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“Contemporary Venus has no oceans, and water vapor is present in the venusian atmosphere at a concentration of only ∼30 ppmv (parts per million by volume; Meadows and Crisp, 1996).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Meadows and Crisp, 1996
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Reinhard, C. T., Olson, S. L., Schwieterman, E. W., & Lyons, T. W. (2017) · Astrobiology · doi:10.1089/ast.2016.1598 · Cited by 93
The deep atmosphere of Venus and the possible role of density-driven separation of CO2 and N2
Lebonnois, S., & Schubert, G. (2017) · Nature Geoscience · doi:10.1038/ngeo2971 · Cited by 90
DETECTING AND CONSTRAINING N2ABUNDANCES IN PLANETARY ATMOSPHERES USING COLLISIONAL PAIRS
Schwieterman, E. W., Robinson, T. D., Meadows, V. S., Misra, A., & Domagal-Goldman, S. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/810/1/57 · Cited by 100
“The SMART model, developed by D. Crisp, is the core radiative transfer engine of the VPL spectral Earth model (Meadows & Crisp 1996; Crisp 1997).”
MethodSelf-citationNear‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere
Piccioni, G., Zasova, L. V., Migliorini, A., Drossart, P., Shakun, A. V., Muñoz, A. G., Mills, F. P., & Cardesín‐Moinelo, A. (2009) · Journal of Geophysical Research Atmospheres · doi:10.1029/2008je003133 · Cited by 88
THE EFFECTS OF REFRACTION ON TRANSIT TRANSMISSION SPECTROSCOPY: APPLICATION TO EARTH-LIKE EXOPLANETS
Misra, A., Meadows, V., & Crisp, D. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/792/1/61 · Cited by 83
Self-citationRadiative forcing at high concentrations of well‐mixed greenhouse gases
Byrne, B., & Goldblatt, C. (2013) · Geophysical Research Letters · doi:10.1002/2013gl058456 · Cited by 96
VIRTIS emissivity of Alpha Regio, Venus, with implications for tessera composition
Gilmore, M. S., Mueller, N. T., & Helbert, J. (2015) · Icarus · doi:10.1016/j.icarus.2015.04.008 · Cited by 86
Organic Haze as a Biosignature in Anoxic Earth-like Atmospheres
Arney, G., Domagal-Goldman, S. D., & Meadows, V. (2017) · Astrobiology · doi:10.1089/ast.2017.1666 · Cited by 85
Self-citationUsing Dimers to Measure Biosignatures and Atmospheric Pressure for Terrestrial Exoplanets
Misra, A., Meadows, V., Claire, M., & Crisp, D. (2014) · Astrobiology · doi:10.1089/ast.2013.0990 · Cited by 84
Self-citationNonphotosynthetic Pigments as Potential Biosignatures
Schwieterman, E. W., Cockell, C. S., & Meadows, V. (2015) · Astrobiology · doi:10.1089/ast.2014.1178 · Cited by 77
Self-citationInfrared Transmission Spectra for Extrasolar Giant Planets
Tinetti, G., Liang, M., Vidal‐Madjar, A., Ehrenreich, D., Etangs, A. L. D., & Yung, Y. L. (2006) · The Astrophysical Journal · doi:10.1086/510716 · Cited by 82
Helbert, J., Mueller, N. T., Kostama, P., Marinangeli, L., Piccioni, G., & Drossart, P. (2008) · Geophysical Research Letters · doi:10.1029/2008gl033609 · Cited by 81
Hydroxide Salts in the Clouds of Venus: Their Effect on the Sulfur Cycle and Cloud Droplet pH
Rimmer, P. B., Jordan, S., Constantinou, T., Woitke, P., Shorttle, O., Hobbs, R., & Paschodimas, A. (2021) · The Planetary Science Journal · doi:10.3847/psj/ac0156 · Cited by 82
Composition of the atmosphere of Venus below the clouds
Bézard, B., & de Bérgh, C. (2007) · Journal of Geophysical Research Atmospheres · doi:10.1029/2006je002794 · Cited by 79
Water vapor abundance near the surface of Venus from Venus Express/VIRTIS observations
Bézard, B., Tsang, C., Carlson, R. W., Piccioni, G., Marcq, E., & Drossart, P. (2009) · Journal of Geophysical Research Atmospheres · doi:10.1029/2008je003251 · Cited by 79
Hasekamp, O., & Butz, A. (2008) · Journal of Geophysical Research Atmospheres · doi:10.1029/2008jd010379 · Cited by 77
Venus Atmospheric Thermal Structure and Radiative Balance
Limaye, S. S., Grassi, D., Mahieux, A., Migliorini, A., Tellmann, S., & Titov, D. V. (2018) · Space Science Reviews · doi:10.1007/s11214-018-0525-2 · Cited by 77
Detectability of Red-Edge-shifted Vegetation on Terrestrial Planets Orbiting M Stars
Tinetti, G., Rashby, S., & Yung, Y. L. (2006) · The Astrophysical Journal · doi:10.1086/505746 · Cited by 75
The composition of the atmosphere of Venus below 100km altitude: An overview
de Bérgh, C., Мороз, В. І., Taylor, F. W., Crisp, D., Bézard, B., & Zasova, L. (2006) · Planetary and Space Science · doi:10.1016/j.pss.2006.04.020 · Cited by 75
Self-citationChemical composition of Venus atmosphere and clouds: Some unsolved problems
Krasnopolsky, V. A. (2006) · Planetary and Space Science · doi:10.1016/j.pss.2006.04.019 · Cited by 74
The temperature of the Venus mesosphere from O2 (aΔg1) airglow observations
BAILEY, J., Meadows, V., Chamberlain, S., & Crisp, D. (2008) · Icarus · doi:10.1016/j.icarus.2008.04.007 · Cited by 73
Self-citationDetecting Ocean Glint on Exoplanets Using Multiphase Mapping
Lustig‐Yaeger, J., Meadows, V., Mendoza, G. T., Schwieterman, E. W., Fujii, Y., Luger, R., & Robinson, T. D. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaed3a · Cited by 73
Self-citationIgnatiev, N., Moroz, V. I., Moshkin, B. E., Ekonomov, A. P., Gnedykh, V. I., Grigoriev, A. V., & Khatuntsev, I. V. (1997) · Planetary and Space Science · doi:10.1016/s0032-0633(96)00143-2 · Cited by 72
Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Wogan, N. F., Catling, D. C., Zahnle, K. J., & Lupu, R. (2023) · The Planetary Science Journal · doi:10.3847/psj/aced83 · Cited by 81
Mischna, M. A., Lee, C., & Richardson, M. I. (2012) · Journal of Geophysical Research Atmospheres · doi:10.1029/2012je004110 · Cited by 78
Detection of Sub-Micron Radiation from the Surface of Venus by Cassini/VIMS
Baines, K. H., Bellucci, G., Bibring, J., Brown, R. H., Buratti, B. J., Bussoletti, E., Capaccioni, F., Cerroni, P., Clark, R. N., Coradini, A., et al. (2000) · Icarus · doi:10.1006/icar.2000.6519 · Cited by 72
Marcq, E. (2011) · Journal of Geophysical Research Atmospheres · doi:10.1029/2011je003912 · Cited by 71
Comparative Climatology of Terrestrial Planets
Mackwell, S., Simon-miller, A., Harder, J., & Bullock, M. (2013) · University of Arizona Press eBooks · doi:10.2458/azu_uapress_9780816530595 · Cited by 100
Haus, R., & Arnold, G. E. (2010) · Planetary and Space Science · doi:10.1016/j.pss.2010.08.001 · Cited by 68
Natraj, V., Jiang, X., Shia, R., Huang, X., Margolis, J. S., & Yung, Y. L. (2005) · Journal of Quantitative Spectroscopy and Radiative Transfer · doi:10.1016/j.jqsrt.2004.12.024 · Cited by 68
Metadata
- Authors
- Meadows, V. S., & Crisp, D.
- ORCID
- Crisp, D.
- Venue
- Journal of Geophysical Research: Planets
- Publisher
- American Geophysical Union (AGU)
- Published
- 1996-02
- Volume
- 101
- Issue
- E2
- Pages
- 4595-4622
- ISSN
- 0148-0227 (ISSN-L)
- OpenAlex
- W1982912142
- Cited by
- 354
- References
- 63
- Citations by year
- 2026: 8 · 2025: 12 · 2024: 16 · 2023: 19 · 2022: 14 · 2021: 9 · 2020: 13 · 2019: 21 · 2018: 13 · 2017: 17 · 2016: 11 · 2015: 17 · 2014: 17 · 2013: 15 · 2012: 11
- FWCI
- 5.39
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Journal of Geophysical Research Atmospheres (publishedVersion)
- Topics
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Planetary Science and Exploration
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- water vapor abundance, atmospheric lapse rate, static stability, CO2 atmosphere, Rayleigh scattering, Mie scattering, surface emissivity, surface topography, radiative transfer modeling, Venus atmosphere, thermal structure, Anglo-Australian Telescope
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