Io’s atmosphere
01 Jan 2007-pp 231-264
About: The article was published on 2007-01-01. It has received 37 citations till now. The article focuses on the topics: Atmosphere & Solar zenith angle.
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TL;DR: The gas-phase chemistry in extraterrestrial space that is driven by reactions with atomic and molecular ions is reviewed, not only the observation, distribution and reactions of ions in space, but also laboratory-based experimental and theoretical methods for studying these ions.
Abstract: We review the gas-phase chemistry in extraterrestrial space that is driven by reactions with atomic and molecular ions. Ions are ubiquitous in space and are potentially responsible for the formation of increasingly complex interstellar molecules. Until recently, positively charged atoms and molecules were the only ions known in space; however, this situation has changed with the discovery of various molecular anions. This review covers not only the observation, distribution and reactions of ions in space, but also laboratory-based experimental and theoretical methods for studying these ions. Recent results from space-based instruments, such as those on the Cassini-Huygens space mission and the Herschel Space Observatory, are highlighted.
219 citations
TL;DR: The PLS data provided a survey of the plasma properties between approx 5 and 30 Jupiter radii [R(sub J)] in the equatorial region as mentioned in this paper, showing that the density decreases with radial distance by nearly 5 orders of magnitude.
Abstract: The plasma science (PLS) Instrument on the Galileo spacecraft (orbiting Jupiter from December 1995 to September 2003) measured properties of the ions that were trapped in the magnetic field The PLS data provide a survey of the plasma properties between approx 5 and 30 Jupiter radii [R(sub J)] in the equatorial region We present plasma properties derived via two analysis methods: numerical moments and forward modeling We find that the density decreases with radial distance by nearly 5 orders of magnitude from approx 2 to 3000 cm(exp-3) at 6R(sub j) to approx 005cm(sub -3) at 30 R(sub j) The density profile did not show major changes from orbit to orbit, suggesting that the plasma production and transport remained constant within about a factor of 2 The radial profile of ion temperature increased with distance which implied that contrary to the concept of adiabatic cooling on expansion, the plasma heats up as it expands out from Io's orbit (where TI is approx60-80 eV) at approx 6R(sub j) to a few keV at 30R(sub j)There does not seem to be a long-term, systematic variation in ion temperature with either local time or longitude This latter finding differs from earlier analysis of Galileo PLS data from a selection of orbits Further examination of all data from all Galileo orbits suggests that System Ill variations are transitory on timescales of weeks, consistent with the modeling of Cassini Ultraviolet Imaging Spectrograph observations The plasma flow is dominated by azimuthal flow that is between 80% and 100% of corotation out to 25 R(sub j)
85 citations
77 citations
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TL;DR: In this paper, it was shown that intrusion of silicate magma into buried SO2 deposits can create the required conditions for high entropy eruptions which proceed entirely in the vapor phase.
Abstract: We suggest that Io's eruptive activity may include a class of previously undetected SO2 geysers. The thermodynamic models for the eruptive plumes discovered by Voyager 'involve low to moderate entropy SO2 eruptions. The resulting plumes are a mixture of solid and gas which emerge from the vent and follow essentially ballistic trajectories. We show that intrusion of silicate magma into buried SO2 deposits can create the required conditions for high entropy eruptions which proceed entirely in the vapor phase. These purely gaseous plumes would have been invisible to Voyager's instruments. Hence, we call them "stealth" plumes. Such eruptions could explain the "patchy" SO2 atmosphere inferred from recent UV and micro-wave spectral observations. The magma intrusion rate required to support the required gas production for these plumes is a negligible fraction of estimated global magma intrusion rates.
59 citations
TL;DR: An extensive set of HI Lyman-α images obtained with the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) from 1997-2001 has been analyzed to provide information about the spatial and temporal character of Io's SO2 atmosphere as mentioned in this paper.
57 citations
References
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Kitt Peak National Observatory1, University of Southern California2, Planetary Science Institute3, Jet Propulsion Laboratory4, University of Michigan5, Johns Hopkins University6, Centre national de la recherche scientifique7, United States Naval Research Laboratory8, York University9, Harvard University10
TL;DR: The observed resonance scattering of solar hydrogen Lyman α by the atmosphere of Jupiter and the solar occultation experiment suggest a hot thermosphere (≥ 1000 K) wvith a large atomic hydrogen abundance.
Abstract: The global hydrogen Lyman alpha, helium (584 angstroms), and molecular hydrogen band emissions from Saturn are qualitatively similar to those of Jupiter, but the Saturn observations emphasize that the H(2) band excitation mechanism is closely related to the solar flux. Auroras occur near 80 degrees latitude, suggesting Earth-like magnetotail activity, quite different from the dominant Io plasma torus mechanism at Jupiter. No ion emissions have been detected from the magnetosphere of Saturn, but the rings have a hydrogen atmosphere; atomic hydrogen is also present in a torus between 8 and 25 Saturn radii. Nitrogen emission excited by particles has been detected in the Titan dayglow and bright limb scans. Enhancement of the nitrogen emission is observed in the region of interaction between Titan's atmosphere and the corotating plasma in Saturn's plasmasphere. No particle-excited emission has been detected from the dark atmosphere of Titan. The absorption profile of the atmosphere determined by the solar occultation experiment, combined with constraints from the dayglow observations and temperature information, indicate that N(2) is the dominant species. A double layer structure has been detected above Titan's limb. One of the layers may be related to visible layers in the images of Titan.
755 citations
Book•
01 Jan 2004
TL;DR: In this paper, the authors present a model for the formation and evolution of the inner and outer clouds of the Jovian satellite system, including the formation of the outer clouds.
Abstract: Preface 1. Introduction F. Bagenal, T. E. Dowling and W. B. McKinnon 2. The origin of Jupiter J. I. Lunine, A. Corandini, D. Gautier, T. C. Owen and G. Wuchterl 3. The interior of Jupiter T. Guillot, D. J. Stevenson, W. B. Hubbard and D. Saumon 4. The composition of the atmosphere of Jupiter F. W. Taylor, S. K. Atreya, Th. Encrenaz, D. M. Hunten, P. G. J. Irwin and T. C. Owen 5. Jovian clouds and haze R. A. West, K. H. Baines, A. J. Friedson, D. Banfield, B. Ragent and F. W. Taylor 6. Dynamics of Jupiter's atmosphere A. P. Ingersoll, T. E. Dowling, P. J. Gierasch, G. S. Orton, P. L. Read, A. Sanchez-Lavega, A. P. Showman, A. A. Simon-Miller and A. R. Vasavada 7. The stratosphere of Jupiter J. I. Moses, T. Fouchet, R. V. Yelle, A. J. Friedson, G. S. Orton, B. Bezard, P. Drossart, G. R. Gladstone, T. Kostiuk and T. A. Livengood 8. Lessons from Shoemaker-Levy 9 about Jupiter and planetary impacts J. Harrington, I. de Pater, S. H. Brecht, D. Deming, V. Meadows, K. Zahnle and P. D. Nicholson 9. Jupiter's thermosphere and ionosphere R. V. Yelle and S. Miller 10. Jovian dust: streams, clouds and rings H. Kruger, M. Horanyi, A. V. Krivov and A. L. Graps 11. Jupiter's ring-moon system J. A. Burns, D. P. Simonelli, M. R. Showalter, D. P. Hamilton, C. C. Porco, H. Throop and L. W. Esposito 12. Jupiter's outer satellites and trojans D. C. Jewitt, S. Sheppard and C. Porco 13. Interior composition, structure and dynamics of the Galilean satellites G. Schubert, J. D. Anderson, T. Spohn and W. B. McKinnon 14. The lithosphere and surface of Io A. S. McEwen, L. P. Keszthelyi, R. Lopes, P. M. Schenk and J. R. Spencer 15. Geology of Europa R. Greeley, C. F. Chyba, J. W. Head III, T. B. McCord, W. B. McKinnon, R. T. Pappalardo and P. Figueredo 16. Geology of Ganymede R. T. Pappalardo, G. C. Collins, J. W. Head III, P. Helfenstein, T. B. McCord, J. M. Moore, L. M. Procktor, P. M. Shenk and J. R. Spencer 17. Callisto J. M. Moore, C. R. Chapman. E. B. Bierhaus, R. Greeley, F. C. Chuang, J. Klemaszewski, R. N. Clark, J. B. Dalton, C. A. Hibbitts, P. M. Schenk, J. R. Spencer and R. Wagner 18. Ages and interiors: the cratering record of the Galilean satellites P. M. Schenk, C. R. Chapman, K. Zahnle and J. M. Moore 19. Satellite atmospheres M. A. McGrath, E. Lellouch, D. F. Strobel, P. D. Feldman and R. E. Johnson 20. Radiation effects on the surfaces of the Galilean satellites R. E. Johnson, R. W. Carlson, J. F. Cooper, C. Paranicas, M. H. Moore and M. C. Wong 21. Magnetospheric interactions with satellites M. G. Kivelson, F. Bagenal, W. S. Kurth, F. M. Neubauer, C. Paranicas and J. Saur 22. Plasma interactions of Io with its plasma torus J. Saur, F. M. Neubauer, J. E. P. Connerney, P. Zarka and M. G. Kivelson 23. The Io neutral clouds and plasma torus N. Thomas, F. Bagenal, T. W. Hill and J. K. Wilson 24. The configuration of Jupiter's magnetosphere K. K. Khurana, M. G. Kivelson, V. M. Vasyliunas, N. Krupp, J. Woch, A. Lagg, B. H. Mauk and W. S. Kurth 25. Dynamics of the Jovian magnetosphere N. Krupp, V. M. Vasyliunas, J. Woch, A. Lagg, K. K. Khurana, M. G. Kivelson, B. H. Mauk, E. C. Roelof, D. J. Williams, S. M. Krimigis, W. S. Kurth, L. A. Frank and W. R. Paterson 26. Jupiter's Aurora J. T. Clarke, D. Grodent, S. W. H. Cowley, E. J. Bunce, P. Zarka, J. E. P. Connerney and T. Satoh 27. Jupiter's inner radiation belts S. J. Bolton, R. M. Thorne, S. Bourdarie, I. de Pater and B. Mauk Appendix 1. Maps and spectra of Jupiter and the Galilean satellites J. R. Spencer, R. W. Carlson, T. L. Becker and J. S. Blue Appendix 2. Planetary parameters J. W. Weiss Index.
486 citations
Book•
01 Jan 1982
TL;DR: In this article, the authors describe the geology of Ganymede, E.M.Shoemaker and R.F.Schaber volcanic eruption plumes on Lo, G.C.Sinton Lo's surface - its phase composition and influence on Lo's atmosphere and Jupiter's magnetosphere, F.Fanale et al.
Abstract: The rings of Jupiter, D.C.Jewitt orbital evolution of the Galilean satellites, R.Greenberg structure and thermal evolution of the Galilean satellites, P.M.Cassen the outer satellites of Jupiter, D.P.Cruikshank et al Amalthea, P.Thomas and J.Veverka composition of the surfaces of the Galilean satellites, G.T.Sill and R.N.Clark radar properties of Europa, Ganymede, and Callisto, S.J.Ostro interpreting the cratering record - Mercury to Ganymede and Callisto, A.Woronow et al cratering time scales for the Galilean satellites, E.M.Shoemaker and R.F.Wolfe experimental simulation of impact cratering on icy satellites, R.Greeley et al craters and basins of Ganymede and Callisto - morphological indicators of crustal evolution, Q.R.Passey and E.M.Shoemaker the geology of Ganymede, E.M.Shoemaker et al the geology of Europa, B.K.Lucchitta and L.A.Soderblom the geology of Lo, G.G.Schaber volcanic eruption plumes on Lo, R.G.Strom and N.M.Schneider volcanic eruptions on Lo - implications for surface evolution and mass loss, T.V.Johnson and L.A.Soderblom dynamics and thermodynamics of volcanic eruptions - implications for the plumes on Lo, S.W.Kieffer hot spots of Lo, J.C.Pearl and W.M.Sinton Lo's surface - its phase composition and influence on Lo's atmosphere and Jupiter's magnetosphere, F.P. Fanale et al the atmospheres of Lo and other satellites, S.Kumar and D.M.Hunten emissions from neutrals and lons in the Jovian magnetosphere, C.B.Pilcher and D.F.Strobel in situ observations of Lo torus plasma, J.D.Sullivan and G.L.Siscoe origin and evolution of the Jupiter satellite system, J.B.Pollack and F.Fanale. Appendix: cartography and nomenclature for the Galilean satellites, M.E.Davies.
325 citations
TL;DR: In this paper, the identification of gaseous sulfur dioxide on Io by Voyager 1 is reported, and preliminary upper limits for other atmospheric gases are presented, with a depletion of hydrogen, carbon and nitrogen.
Abstract: The identification of gaseous sulfur dioxide on Io by Voyager 1 is reported, and preliminary upper limits for other atmospheric gases are presented. Averaged spectra taken by the Voyager IRIS experiment in the range of 1,000 to 1,200/cm are interpreted as containing three fundamental sulfur dioxide bands, with intensities most nearly corresponding to an atmospheric model with a sulfur dioxide abundance of 0.2 cm atm. Upper limits for COS, CS2, SO3, H2S, CO2, O3, N2O, H2O, CH4, NH3 and HC1, not detected in the spectra, were calculated on the basis of the radiative transfer equation for temperatures of 130 and 250 K; a depletion of hydrogen, carbon and nitrogen is noted. It is suggested that a SO2 outgassing from a cooling sulfur extrusion is the major source of the observed atmospheric SO2.
278 citations
TL;DR: Jupiterward of the Io plasma torus, a cold, corotating plasma was observed and the energylcharge spectra show well-resolved, heavy-ion peaks at mass-to-charge ratios A/Z* = 8, 16, 32, and 64.
Abstract: Extensive measurements of low-energy positive ions and electrons were made throughout the Jupiter encounter of Voyager 1. The bow shock and magnetopause were crossed several times at distances consistent with variations in the upstream solar wind pressure measured on Voyager 2. During the inbound pass, the number density increased by six orders of magnitude between the innermost magnetopause crossing at approximately 47 Jupiter radii and near closest approach at approximately 5 Jupiter radii; the plasma flow during this period was predominately in the direction of corotation. Marked increases in number density were observed twice per planetary rotation, near the magnetic equator. Jupiterward of the Io plasma torus, a cold, corotating plasma was observed and the energy/charge spectra show well-resolved, heavy-ion peaks at mass-to-charge ratios equal to 8, 16, 32, and 64.
239 citations