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The atmosphere and ionosphere of Io

McElroy, Michael B. and Yung, Yuk Ling (1975) The atmosphere and ionosphere of Io. Astrophysical Journal, 196 (1). pp. 227-250. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20140924-085334547

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Abstract

A variety of models for Io's atmosphere, ionosphere, surface, and environment are developed and discussed in the context of recent observational data. The sodium emission detected by Brown appears to require a collisional excitation process in Io's atmosphere, and the extended sodium emission measured by Trafton et al. may require scattering of the planetary radiation by an extended sodium cloud. The sodium is presumably present initially in bound form on Io's surface and may be released by the sputtering mechanism suggested by Matson et al. The ionosphere detected by the radio occultation experiment on Pioneer 10 could be attributed to photoionization of atmospheric sodium if Io's atmosphere could sustain significant vertical motions, of order 1 s^(-1) directed up during the day, down at night. Vertical motions of this magnitude could be driven by condensation of atmospheric NH_3. The total density of gas at Io's surface appears to lie in the range 10^(10)-10^(12) molecules cm^(-3). Corpuscular ionization could play an additional role for the Ionosphere. In this case the satellite should exhibit an exceedingly bright, ~ 10 kR, airglow at Lɑ. The incomplete hydrogen torus observed by Judge and Carlson in the vicinity of Io requires a large supply of hydrogen from the satellite's atmosphere. The escape flux should be of order 10^(11) cm^(-2) s^(-1) and could be maintained by photolysis of atmospheric NH_3. The observed geometry of the hydrogen torus appears to require a surprisingly short lifetime, ~ 10^5 s, for neutral hydrogen near Io's orbit, and may indicate the presence of a large flux, ~ 10^9 cm ^(-2) s^(-1), of low-energy protons in Jupiter's magnetosphere. Implications of the hydrogen torus for the energy and mass balance of Jupiter's magnetosphere are discussed briefly, and observational programs are identified which might illuminate present uncertainties in our understanding of Io.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://adsabs.harvard.edu/abs/1975ApJ...196..227MADSArticle
http://dx.doi.org/10.1086/153408DOIArticle
Additional Information:© 1975 The American Astronomical Society. Provided by the NASA Astrophysics Data System. Received 1974 May 30; revised 1974 August 23. We are indebted to R. W. Carlson, D. L. Judge, A. Kliore, S. I. Rasool, J. A. Simpson, and J. H. Wolfe for informative discussions of the Pioneer JO data. We acknowledge also the patience and stimulation of various colleagues, particularly R. A. Brown, H. Ehrenreich, R. M. Goody, and S. C. Wofsy, who bore with us during the course of this research. The work was supported by the Atmospheric Sciences Section of the National Science Foundation under grant GA-33990X to Harvard University. We also acknowledge partial support from the National Aeronautics and Space Administration contract NGL 22-007-228 to Harvard University.
Funders:
Funding AgencyGrant Number
NSFGA-33990X
NASANGL 22-007-228
Subject Keywords:atmospheres, planetary, Jupiter, satellites
Record Number:CaltechAUTHORS:20140924-085334547
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140924-085334547
Official Citation:The atmosphere and ionosphere of Io McElroy, M. B.; Yung, Y. L. Astrophysical Journal, vol. 196, Feb. 15, 1975, pt. 1, p. 227-250
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:49975
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:24 Sep 2014 16:15
Last Modified:13 Feb 2019 18:06

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