Occultation Experiment: Results of the First Direct Measurement of Mars's Atmosphere and Ionosphere

Kliore, A. J.; Cain, D. L.; Levy, G. S.; Eshleman, V. R.; Fjeldbo, G.; Drake, F. D.

doi:10.1126/science.149.3689.1243

Cited by 323 publications

(135 citation statements)

References 3 publications

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“…The feasibility of the radio occultation technique to obtain atmospheric profiles of temperature and density with altitude was first demonstrated by Mariner 4 at Mars (Kliore et al 1965) and then at Venus by Mariner 5 (Kliore et al 1967) using both one way (spacecraft to Earth), and two way (Earth to spacecraft to Earth) occultations (Howard et al 1974), generally at two frequencies (X and S band). Venera 9/10 occultations at 32 cm (Kolosov et al 1978;) and 15/16 at 5 and 13 cm wavelengths (Yakovlev et al 1987) orbiters also obtained radio occultation profiles by using these radio frequencies.…”

Section: Radio Occultations: Post Pioneer Venus and Pre-venus Expressmentioning

confidence: 99%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet's extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in [1411][1412][1413][1414] 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595-4622, 1996) from 1 μm observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.

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Section: Radio Occultations: Post Pioneer Venus and Pre-venus Expressmentioning

confidence: 99%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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“…Venus, Mars) and ionosphere (e.g. Fjeldbo and Eshelman, 1965, Kliore et al, 1965, Fjeldbo et al, 1971, Kliore and Patel, 1982, Lindal et al, 1983. The GPS/MET experiment on board the Low Earth Orbiter (LEO) Microlab 1 (launched on 3 April 1995) consists of a GPS receiver to obtain atmospheric refractivities during the rise or set of the LEO satellite relative to one of the 24 GPS satellites (Kursinski et al, 1997).…”

Section: Introductionmentioning

confidence: 99%

Validation of a regional weather forecast model with GPS data

Johnsen

Rockel

2001

Physics and Chemistry of the Earth, Part B: Hydrology, Oceans a

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“…The dotted horizontal line represents the partial pressure of water on the present martian surface, calculated using the abundance of H 2 O in the atmosphere Owen et al, 1977, Jakosky and Phillips, 2001and Bish et al, 2003 and the total atmospheric pressure (Kliore et al, 1965). The dotted vertical line represents the average surface temperature at the equator.…”

Section: Thermodynamic Calculations and Discussionmentioning

confidence: 99%

Acknowledgements to references

1981

Arch. Microbiol.

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Jarosite, a potassium (sodium) iron sulphate hydrated mineral, has recently been identified on the martian surface by the Opportunity rover. Using recent thermochemical data [Drouet and Navrotsky, 2003, Geochim. Cosmochim. Acta 67, 2063-2076 Forray et al., 2005, Geochim. Cosmochim. Acta, in press], we calculate the equilibrium decomposition curve of jarosite and show that it is thermodynamically stable under most present martian pressures and temperatures. Its stability makes jarosite potentially useful to retain textural, chemical, and isotopic evidence of past history, including possible biological activity, on Mars.

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Occultation Experiment: Results of the First Direct Measurement of Mars's Atmosphere and Ionosphere

Cited by 323 publications

References 3 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

Validation of a regional weather forecast model with GPS data

Acknowledgements to references

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