The DOI matches its Crossref record; 63 of the 63 references it cites were found in a registry or an index.
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
Citations
Cites
Stamnes, K. H., Tsay, S. C., Wiscombe, W. J., & Jayaweera, K. O. L. F. (1988) · Applied Optics · doi:10.1364/ao.27.002502 · Cited by 3,353
Improved Mie scattering algorithms
Wiscombe, W. J. (1980) · Applied Optics · doi:10.1364/ao.19.001505 · Cited by 1,690
Atmospheric Radiation: Theoretical Basis
Goody, R. M., & Yung, Y. L. (1989) · Cited by 809
Line shape and the water vapor continuum
Clough, S. A., Kneizys, F. X., & Davies, R. W. (1989) · Atmospheric Research · doi:10.1016/0169-8095(89)90020-3 · Cited by 703
Optical Constants of Sulfuric Acid; Application to the Clouds of Venus?
Palmer, K. F., & Williams, D. (1975) · Applied Optics · doi:10.1364/ao.14.000208 · Cited by 606
Optimized computation of the voigt and complex probability functions
Humlíček, J. (1982) · Journal of Quantitative Spectroscopy and Radiative Transfer · doi:10.1016/0022-4073(82)90078-4 · Cited by 498
Near-Infrared Light from Venus' Nightside: A Spectroscopic Analysis
Pollack, J. B., Dalton, J. B., Grinspoon, D. H., Wattson, R. B., Freedman, R., Crisp, D., Allen, D. A., Bézard, B., de Bérgh, C., Giver, L. P., et al. (1993) · Icarus · doi:10.1006/icar.1993.1055 · Cited by 366
Self-citationEnergy levels, intensities, and linewidths of atmospheric carbon dioxide bands
Rothman, L. S., Hawkins, R. L., Wattson, R. B., & Gamache, R. R. (1992) · Journal of Quantitative Spectroscopy and Radiative Transfer · doi:10.1016/0022-4073(92)90119-o · Cited by 319
The deep atmosphere of Venus revealed by high-resolution nightside spectra
Bézard, B., de Bérgh, C., Crisp, D., & Maillard, J. P. (1990) · Nature · doi:10.1038/345508a0 · Cited by 242
Self-citationCloud structure on the dark side of Venus
Allen, D. A., & Crawford, J. W. (1984) · Nature · doi:10.1038/307222a0 · Cited by 222
Research works printed but not linked: 10
- Allen D. A. IAU Circ. 4962 Int. Astron. Union Cambridge MA 1990.
- Barton J. R., 1992, Proceedings of the 10th Symposium on Photoelectronic Image Devices, 147
- Carlson R. W., 1993, (abstract), Galileo/NIMS near‐infrared thermal imagery of the surface of Venus, Proc. Lunar Planet. Sci. Conf., 253
- Donahue T. M., 1992, International Colloquium on Venus, 29
- Meadows V. S. Infrared Observations with IRIS: From Planets to Galaxies Ph.D. thesis Univ. of Sydney Sydney N.S.W Australia 1994.
- Meadows V. S., 1992, International Colloquium on Venus, 70
- Moroz V. I., Panorama of the Venusian surface: Some conclusions concerning boundary layer of atmosphere, Kosm. Issled.
- Moroz V. I., 1983, Venus, 45
- Seiff A., 1983, Venus, 215
- Zahn U., 1983, Venus, 299
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HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES
Kopparapu, R. K., Ramirez, R., Kasting, J. F., Eymet, V., Robinson, T. D., Mahadevan, S., Terrien, R. C., Domagal-Goldman, S., Meadows, V., & Deshpande, R. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/765/2/131 · Cited by 1,615
“D line-by-line radiative transfer model SMART (Spectral Mapping Atmospheric Radiative Transfer) developed by D. Crisp (Meadows & Crisp 1996; Crisp 1997).”
MethodSelf-citationMolecfit: A general tool for telluric absorption correction
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Self-citationBiosignatures from Earth-Like Planets Around M Dwarfs
Segura, A., Kasting, J. F., Meadows, V., Cohen, M., Scalo, J., Crisp, D., Butler, R. A. H., & Tinetti, G. (2005) · Astrobiology · doi:10.1089/ast.2005.5.706 · Cited by 524
Self-citationExoplanet Biosignatures: A Review of Remotely Detectable Signs of Life
Schwieterman, E. W., Kiang, N. Y.-L., Parenteau, M. N., Harman, C. E., DasSarma, S., Fisher, T. M., Arney, G., Hartnett, H. E., Reinhard, C. T., Olson, S. L., et al. (2017) · eScholarship (California Digital Library) · Cited by 452
Self-citation
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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