The Atmospheres of the Planets

Urey, Harold C.

doi:10.1007/978-3-642-45929-0_3

Cited by 41 publications

(9 citation statements)

References 99 publications

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“…The partial pressure of water deduced for the surface of Mars from the data of Kaplan et al (36) is in agreement with that previously estimated by Urey (27). The low value of PH,O on Mars has been attributed by Adamcik (37) to a buffering action of the hematite-goethite (Fe2O80H) equilibrium.…”

Section: Mars Moon and Earthsupporting

confidence: 89%

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Chemistry in planetology

Mueller¹

1965

J. Chem. Educ.

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Section: Mars Moon and Earthsupporting

confidence: 89%

“…We must however consider the possibility of modification of the thermochemical abundances by photochemical reactions in the upper atmosphere(27,28). At 700°1< the value is approximately atmospheres as determined from thermochemical data, so that oxygen should be very depleted in the Venus atmosphere if thermochemical equilibria are in control.…”

mentioning

confidence: 99%

Chemistry in planetology

Mueller¹

1965

J. Chem. Educ.

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“…Photodissociation of atmospheric water vapor, followed by escape of H-atoms from the upper atmosphere might be considered as a source of excess atmospheric oxygen. The calculations of HARTECK & JENSEN (1948), KUIPER (1952), andUREY (1959) have shown that oxygen in the earth's atmosphere may originate in part from such a source. However, production of oxygen in the Venus atmosphere in this way should be negligible due to the combination of higher total pressure and very low temperature at the cloud layer which would limit the transport of water vapor through the atmosphere.…”

Section: (15)mentioning

confidence: 99%

Radiation equilibria pertinent to planetary atmospheres

Harteck¹,

Reeves²,

Thompson³

et al. 1966

Tellus A: Dynamic Meteorology and Oceanography

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Radiation equilibria due to ionizing radiation or ultraviolet light, or both, on systems such as air, oxygen, carbon dioxide, and their mixtures are of major importance to planetary atmospheres. To investigate the radiation equilibria in the ultraviolet region, a special "Bromine" lemp has been developed which gives 10'' quanta/sec at 1582 and 1633 A where the latter is the most intense Br line. Since the absorption coefficients of 0,, CO,, 0, and other gases are substantial at these wavelengths, radiation equilibria can be obtained in reasonable times (between 1 hr and a few days, depending on conditions) in our 500 ml sample volume. Since the temperature can also be varied, the conditions prevailing in any region of an atmosphere can be simulated. The wall effects are negligible for pressures down to a few mm.The irradiation of 0,, CO, CO,, N, and mixtures of these gases are discussed. The effects of trace amounts of water vapor on the equilibria are noted. PAABAqHOHHOE PABHOBECBE, IIPBCYIIJEE IIJIAHETAPHbIM ATMOCQEPAMTellus XVIII (1966), 2

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“…In the next paragraph an upper limit will be set on the sodium influx by comparing it with the maximum allowable influx of neon. Urey [1959] has shown that one can establish an upper limit on the amount of neon coming from the sun by integrating the flux throughout geologic time and comparing it with the amount of neon in the atmosphere at the present time.…”

Section: /•Pik (Private Communication 1961) Howevermentioning

confidence: 99%

“…Therefore, the total amount of neon in the atmosphere represents the maximum integrated influx of neon throughout geologic time (taken as 4 X 109 years). The total amount of neon in the earth's atmosphere is given by Urey [1959] as 2 X 1089 atoms. This represents an upper limit of neon influx of 5 X 10 TM atoms/year.…”

Section: /•Pik (Private Communication 1961) Howevermentioning

confidence: 99%

On the origin of the sodium present in the upper atmosphere

Junge¹,

Oldenberg²,

Wasson³

1962

J. Geophys. Res.

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Various origins are considered for the atmospheric sodium observed in the twilight and nightglow above an altitude of 70 km. The transport of sea salt to these altitudes in sufficient quantities seems impossible except in the unlikely case of complete atomization of the sodium at low altitudes (30 km). Other terrestrial sources seem even more unlikely. The sodium has not accreted from the sun, as shown by a consideration of the amount of neon now present in the atmosphere. Meteoric influx does provide sufficient quantities of atomic sodium at altitudes of 70 km and greater, and is probably the source of the airglow sodium. The influx of micrometeoritic material is capable of providing even more sodium than do the meteors, but there is great uncertainty as to the fraction of this material which vaporizes. Other metals which have been observed in the high atmosphere are Ca, Li, and Mg. However, no conclusions with regard to the origin of these constituents can be drawn from the presently available evidence.

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The Atmospheres of the Planets

Cited by 41 publications

References 99 publications

Chemistry in planetology

Chemistry in planetology

Radiation equilibria pertinent to planetary atmospheres

On the origin of the sodium present in the upper atmosphere

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