Relevant bibliographies by topics / Saturn's atmosphere

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Saturn's atmosphere'

Author: Grafiati
Published: 4 June 2021
Last updated: 15 February 2022

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Journal articles on the topic "Saturn's atmosphere"

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Fletcher, Leigh N. "Saturn's seasonal atmosphere." Astronomy & Geophysics 58, no. 4 (August 1, 2017): 4.26–4.30. http://dx.doi.org/10.1093/astrogeo/atx138.

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Coates, Andrew J. "Interaction of Titan's ionosphere with Saturn's magnetosphere." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 367, no. 1889 (November 20, 2008): 773–88. http://dx.doi.org/10.1098/rsta.2008.0248.

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Titan is the only Moon in the Solar System with a significant permanent atmosphere. Within this nitrogen–methane atmosphere, an ionosphere forms. Titan has no significant magnetic dipole moment, and is usually located inside Saturn's magnetosphere. Atmospheric particles are ionized both by sunlight and by particles from Saturn's magnetosphere, mainly electrons, which reach the top of the atmosphere. So far, the Cassini spacecraft has made over 45 close flybys of Titan, allowing measurements in the ionosphere and the surrounding magnetosphere under different conditions. Here we review how Titan's ionosphere and Saturn's magnetosphere interact, using measurements from Cassini low-energy particle detectors. In particular, we discuss ionization processes and ionospheric photoelectrons, including their effect on ion escape from the ionosphere. We also discuss one of the unexpected discoveries in Titan's ionosphere, the existence of extremely heavy negative ions up to 10 000 amu at 950 km altitude.
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Balcerak, Ernie. "Vortices in Saturn's upper atmosphere." Eos, Transactions American Geophysical Union 95, no. 44 (November 4, 2014): 408. http://dx.doi.org/10.1002/2014eo440016.

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Hall, D. T., P. D. Feldman, J. B. Holberg, and M. A. McGrath. "Fluorescent Hydroxyl Emissions from Saturn's Ring Atmosphere." Science 272, no. 5261 (April 26, 1996): 516–18. http://dx.doi.org/10.1126/science.272.5261.516.

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Ingersoll, Andrew P., Shawn P. Ewald, Kunio M. Sayanagi, and John J. Blalock. "Saturn's Atmosphere at 1-10 Kilometer Resolution." Geophysical Research Letters 45, no. 15 (August 11, 2018): 7851–56. http://dx.doi.org/10.1029/2018gl079255.

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Connerney, J. E. P. "Magnetic connection for Saturn's rings and atmosphere." Geophysical Research Letters 13, no. 8 (August 1986): 773–76. http://dx.doi.org/10.1029/gl013i008p00773.

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Hartle, R. E. "Interaction of Titan's atmosphere with Saturn's magnetosphere." Advances in Space Research 5, no. 4 (January 1985): 321–32. http://dx.doi.org/10.1016/0273-1177(85)90158-9.

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Dandouras, Iannis, Philippe Garnier, Donald G. Mitchell, Edmond C. Roelof, Pontus C. Brandt, Norbert Krupp, and Stamatios M. Krimigis. "Titan's exosphere and its interaction with Saturn's magnetosphere." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 367, no. 1889 (November 20, 2008): 743–52. http://dx.doi.org/10.1098/rsta.2008.0249.

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Titan's nitrogen-rich atmosphere is directly bombarded by energetic ions, due to its lack of a significant intrinsic magnetic field. Singly charged energetic ions from Saturn's magnetosphere undergo charge-exchange collisions with neutral atoms in Titan's upper atmosphere, or exosphere, being transformed into energetic neutral atoms (ENAs). The ion and neutral camera, one of the three sensors that comprise the magnetosphere imaging instrument (MIMI) on the Cassini/Huygens mission to Saturn and Titan, images these ENAs like photons, and measures their fluxes and energies. These remote-sensing measurements, combined with the in situ measurements performed in the upper thermosphere and in the exosphere by the ion and neutral mass spectrometer instrument, provide a powerful diagnostic of Titan's exosphere and its interaction with the Kronian magnetosphere. These observations are analysed and some of the exospheric features they reveal are modelled.
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Fischer, G., S. Y. Ye, J. B. Groene, A. P. Ingersoll, K. M. Sayanagi, J. D. Menietti, W. S. Kurth, and D. A. Gurnett. "A possible influence of the Great White Spot on Saturn kilometric radiation periodicity." Annales Geophysicae 32, no. 12 (December 4, 2014): 1463–76. http://dx.doi.org/10.5194/angeo-32-1463-2014.

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Abstract. The periodicity of Saturn kilometric radiation (SKR) varies with time, and its two periods during the first 5 years of the Cassini mission have been attributed to SKR from the northern and southern hemisphere. After Saturn equinox in August 2009, there were long intervals of time (March 2010 to February 2011 and September 2011 to June 2012) with similar northern and southern SKR periods and locked SKR phases. However, from March to August 2011 the SKR periods were split up again, and the phases were unlocked. In this time interval, the southern SKR period slowed down by ~ 0.5% on average, and there was a large jump back to a faster period in August 2011. The northern SKR period speeded up and coalesced again with the southern period in September 2011. We argue that this unusual behavior could be related to the so-called Great White Spot (GWS), a giant thunderstorm that raged in Saturn's atmosphere around that time. For several months in 2011, the visible head of the GWS had the same period of ~ 10.69 h as the main southern SKR modulation signal. The GWS was most likely a source of intense gravity waves that may have caused a global change in Saturn's thermospheric winds via energy and momentum deposition. This would support the theory that Saturn's magnetospheric periodicities are driven by the upper atmosphere. Since the GWS with simultaneous SKR periodicity measurements have only been made once, it is difficult to prove a physical connection between these two phenomena, but we provide plausible mechanisms by which the GWS might modify the SKR periods.
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Heintz, Andreas, and Eckard Bich. "Thermodynamics in an icy world: The atmosphere and internal structure of Saturn's moon Titan." Pure and Applied Chemistry 81, no. 10 (October 3, 2009): 1903–20. http://dx.doi.org/10.1351/pac-con-08-10-04.

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Thermodynamic principles can be applied for describing the atmospheres and the internal structure of celestial bodies using Saturn's moon Titan as a most appropriate example. Some basic physical data of Titan such as the measured temperature and pressure on its surface, the atmospheric composition, Titan’s density and diameter, and other information allow us to predict further properties which have not been determined directly by measurements. The existence of a liquid phase covering smaller parts of the surface can be confirmed, and the composition of the liquid can be predicted. The change of temperature with the height over the surface and the appearance of clouds and rainfall in the atmosphere consisting essentially of CH4 + N2 mixtures can also be predicted. By developing a new method of calculation of atmospheric scenarios, the chemical history of Titan’s surface and atmosphere can be roughly reconstructed taking into account the known rate of methane destruction caused by radiative absorption of sunlight. Finally, some estimations concerning the material structure and the pressure behavior of Titan’s interior can be made. Only basic knowledge of thermodynamics and physics is required to understand essential features in a strange world that is more than one billion kilometers away from us.
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Dissertations / Theses on the topic "Saturn's atmosphere"

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Cooray, Asantha Roshan. "Stellar occultation observations of Saturn's upper atmosphere." Thesis, Massachusetts Institute of Technology, 1997. http://hdl.handle.net/1721.1/53030.

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Thesis (M.S.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 1997.
Includes bibliographical references (leaves 74-79).
by Asantha Roshan Cooray.
M.S.
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Foust, Jeffrey Alan 1971. "Stellar occultation studies of Saturn's upper atmosphere." Thesis, Massachusetts Institute of Technology, 1999. http://hdl.handle.net/1721.1/9528.

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Thesis (Ph.D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 1999.
Includes bibliographical references (p. 224-230).
The properties of Saturn's upper atmosphere are not well-known despite several spacecraft flybys. However, the region of 1-100 [mu]bar can be studied in detail by observing stellar occultations -- when the planet passes in front of a star -- from ground-based or Earth-orbiting telescopes. We use data from five such occultations: three observed in 1995 by the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST), one observed in 1996 at the NASA Infrared Telescope Facility (IRTF) and one in 1989 observed by a different instrument at the IRTF. The data span latitudes from 52° south to 75 ° north. We fit isothermal models to each data set and also perform numerical inversions. These analyses show that temperatures in the 1-10 [mu]bar range can vary significantly as a function of season and latitude, ranging from 121 to 160 K, in accordance with radiative transfer models for the atmosphere. We also search for evidence of gravity wave saturation in Saturn's upper atmosphere, as seen in other planetary atmospheres, by analyzing the power spectra of temperature and density data and by studying the temperature lapse rate in the atmosphere. Our analysis is consistent with saturated gravity waves for all data sets, although gravity wave saturation is not the sole explanation for the spectra. We take advantage of the wavelength-resolved HST FOS data to study the composition of Saturn's upper atmosphere. We measured the difference in feature times for data taken at two wavelengths, and use the different refractivities of hydrogen and helium, as a function of wavelength to compute the relative amounts of the two elements in the planet's atmosphere. We find that the helium mass fraction is 0.26 ± 0.10, higher than that found using Voyager data, but marginally consistent with theoretical models for the evolution of Saturn's atmosphere, although the large error bars on the results make a definitive conclusion problematic.
by Jeffrey Alan Foust.
Ph.D.
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Fletcher, Leigh Nicholas. "Saturn's atmosphere : structure and composition from Cassini/CIRS." Thesis, University of Oxford, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.445756.

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Koskinen, T. T., J. I. Moses, R. A. West, S. Guerlet, and A. Jouchoux. "The detection of benzene in Saturn's upper atmosphere." AMER GEOPHYSICAL UNION, 2016. http://hdl.handle.net/10150/621596.

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The stratosphere of Saturn contains a photochemical haze that appears thicker at the poles and may originate from chemistry driven by the aurora. Models suggest that the formation of hydrocarbon haze is initiated at high altitudes by the production of benzene, which is followed by the formation of heavier ring polycyclic aromatic hydrocarbons. Until now there have been no observations of hydrocarbons or photochemical haze in the production region to constrain these models. We report the first vertical profiles of benzene and constraints on haze opacity in the upper atmosphere of Saturn retrieved from Cassini Ultraviolet Imaging Spectrograph stellar occultations. We detect benzene at several different latitudes and find that the observed abundances of benzene can be produced by solar-driven ion chemistry that is enhanced at high latitudes in the northern hemisphere during spring. We also detect evidence for condensation and haze at high southern latitudes in the polar night.
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Karkoschka, Erich. "Saturn's atmosphere in the visible and near-infrared, 1986-1989." Diss., The University of Arizona, 1990. http://hdl.handle.net/10150/185074.

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This work describes observations of Saturn's atmosphere in the visible and near infrared (450-1000 nm) including four hydrogen quadrupole lines, 17 methane absorption bands ranging over three orders of magnitude in absorption strength, an ammonia absorption band, and the absolute calibrated continuum spectrum. All observations have complete coverage of Saturn's disk, in latitude as well as in center-to-limb position. The accuracy of the data is comparable or better than previous data. This data set gives a quite complete description of Saturn's atmosphere in the visible and near infrared at the spatial resolution of ground based observations. While the main data were acquired in 1988, small changes between 1986 and 1989 were determined also. An atmospheric model is given which fits all observations within estimated errors. It has clear gas at the top of the atmosphere, an extended haze layer and a reflective cloud at the bottom. Pressure levels and the haze optical depth were determined as a function of latitude. The single scattering albedo spectrum of the particles (most likely ammonia ice crystals) is also given for each latitude. The methane mixing ratio is (3.0 ± 0.6) x 10⁻³, the ammonia mixing ratio is (1.2 + 0.8/-0.6) x 10⁻³ below the ammonia condensation level. Room temperature methane absorption spectra do not fit the observed spectra for any cloud structure. A cold temperature methane absorption spectrum is determined under the assumption that methane band strengths are temperature invariant, but not necessarily the absorption coefficients at each location across the band. It indicates that the absorption coefficients are typically 20-30 per cent stronger in the center of a band and up to a factor of two weaker in the wings. This spectrum should be useful in the interpretation of methane observations of all the giant planets and Titan.
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Feng, Da Sheng. "Recovering the hydrocarbon distributions in Saturn's upper atmosphere through mathematical inversion." Diss., The University of Arizona, 1991. http://hdl.handle.net/10150/185665.

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The spacecraft Voyager 2 UVS occultation experiments measured the ultraviolet absorption properties of the upper atmosphere of Saturn. In the extreme-ultraviolet wavelength region from 1300 Å to 1700 Å, CH₄, C₂H₂, C₂H₄, C₂H₆ and C₄H₂ are the major absorbers in the Saturnian upper atmosphere. In this dissertation, using the linear constrained matrix method, the Saturnian stellar EUV occultation data has been inverted. This results in, for the first time, the number density distributions of the 5 major hydrocarbons over an altitude range from 1030 km to 630 km. The synthetic transmission curves based on these inverted distributions exhibit excellent agreement with the observed transmission curves in all usable wavelength channels. There are two major findings in the Saturnian upper atmosphere from the inverted hydrocarbon profiles: (1) The number densities of CH₄ and C₂H₆ are comparable. It is even likely that there is more C₂H₆ than CH₄ in Saturn's upper atmosphere between 1000 km and 800 km. (2) C₂H₄, rather than C₂H₂, is the 3rd most abundant hydrocarbon. From 1000 km down to 600 km, the number density of C₂H₄ is greater than the number density of C₂H₂. These two findings are generally in conflict with the expectations from photochemical models for the atmospheres of the giant planets.
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Sylvestre, Mélody. "Modélisation numérique de la dynamique atmosphérique de Saturne contrainte par les données Cassini-Huygens." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066446/document.

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L'atmosphère de Saturne subit d'importantes variations saisonnières d'insolation, à cause de son obliquité, de son excentricité et de l'ombre de ses anneaux. Dans la stratosphère (de 20 hPa à 10-4 hPa), les échelles de temps photochimiques et radiatives sont du même ordre de grandeur que la période de révolution de Saturne (29,5 ans). On s'attend donc à mesurer des variations saisonnières et méridiennes significatives de la température et des espèces produites par la photochimie (en particulier C2H6, C2H2 et C3H8) dans cette région. Grâce à sa durée (2004-2017), la mission Cassini est l'occasion inédite de suivre l'évolution saisonnière de l'atmosphère de Saturne.Au cours de ma thèse, j'ai analysé des observations au limbe Cassini/CIRS car elles permettent de sonder à la fois la structure méridienne et verticale de la stratosphère de Saturne. Ainsi, j'ai mesuré les variations saisonnières de la température et des abondances de C2H6, C2H2 et C3H8. J'ai également contribué au développement d'un modèle radiatif-convectif et d'un GCM (Global Climate Model) de l'atmosphère de Saturne. Les prédictions de ces modèles sont comparées avec les températures mesurées avec CIRS, de façon à étudier les processus radiatifs et dynamiques qui contribuent à l'évolution saisonnière. Les simulations numériques réalisées avec ce GCM m'ont également permis d'étudier la propagation des ondes atmosphérique ainsi que les effets de l'ombre des anneaux sur l'atmosphère de Saturne. Par ailleurs, la comparaison entre les distributions de C2H6, C2H2 et C3H8 et des modèles photochimiques (Moses et Greathouse 2005, Hue et al. 2015) donne des indications sur le transport méridien
Saturn's atmosphere undergoes important seasonal variations of insolation, due to its obliquity, its eccentricity and the shadow of its rings. In the stratosphere (from 20 hPa to 10-4 hPa), radiative and photochemical timescales are in the same order as Saturn's revolution period (29.5 ans). Hence, significative seasonal and meridional variations of temperature and photochemical by-products (especially C2H6, C2H2, and C3H8) are expected. Because of its duration (2004-2017), the Cassini mission is an unprecedented opportunity to monitor the seasonal evolution of Saturn's atmosphere. During my PhD, I analysed Cassini/CIRS limb observations as they probe the meridional and vertical structure of Saturn's stratosphere. Hence, I measured seasonal variations of temperature and abundances of C2H6, C2H2, and C3H8. I also contributed to the development of a radiative-convective model and a GCM (Global Climate Model) of Saturn's atmosphere. The predictions of these models are compared with the temperatures measured from CIRS observations, in order to study the radiative and dynamical processes which contribute to the seasonal evolution. Numerical simulations performed with the GCM also allowed me to study atmospheric waves propagation and the effects of rings shadowing in Saturn's atmosphere. Besides, comparison between C2H6, C2H2, and C3H8 distributions and photochemical models (Moses and Greathouse 2005, Hue et al., 2015) give insights on meridional transport
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Fountaine, Timothy. "Saturn's atmosphere : Functional analysis of α-synuclein using RNAi-mediated knockdown in human neuronal cells." Thesis, University of Oxford, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.445757.

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Sinclair, James A. "Seasonal and interannual variability in Saturn's stratosphere." Thesis, University of Oxford, 2014. http://ora.ox.ac.uk/objects/uuid:1ae2289b-a615-4d16-8f01-b13ea10f3bbe.

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The stratosphere of Saturn is highly variable. With an axial tilt of 26.7°, Saturn experiences seasons like Earth and is currently approaching northern summer solstice in 2017. In addition to general seasonal change, previous studies have highlighted that Saturn's stratosphere is host to a range of dynamical phenomena. These processes have an observable effect on the vertical temperature profile and stratospheric concentrations of acetylene (C2H2) and ethane (C2H6), which may be determined or retrieved from thermal infrared observations of Saturn. This thesis presents an analysis of observations of Saturn acquired by Voyager's IRIS (Infrared Interferometer Spectrometer, 180 - 2500 cm-1, Hanel et al.,[1980]) instrument in 1980, Cassini's CIRS (Composite Infrared Spectrometer, 10 - 1400 cm-1, Flasar et al.,[2004]) instrument from 2005 to 2012 and the Celeste spectrometer (400 - 2000 cm-1, Moran et al.,[2007]) on NASA's IRTF (Infrared Telescope Facility) in 2012 in order to track seasonal and interannual changes in Saturn's stratosphere. The concentrations of C2H2 and C2H6 were seen to decrease at 15°S and increase at 25°N from 2005 to 2009/2010. These changes at 15°S and 25°N respectively indicate upward and downward branches associated with cross-equatorial seasonally-reversing Hadley circulation that has been predicted by a general circulation model [Friedson and Moses, 2012]. Strong cooling of up to 17 K at high-southern latitudes from 2005 to 2010 suggests an autumnal weakening of a vortex that appears to form at the pole of the summer hemisphere [Fletcher et al., 2008]. The emergence of a similar northern polar vortex as northern summer solstice approaches was yet to be observed in 2012. Interannual differences in the equatorial temperature structure between 1980 and 2009/2010 suggest Saturn's semiannual oscillation (or SSAO, Fouchet et al. [2008]; Orton et al. [2008]) has been captured in a different phase from one year to the next. This is puzzling since the oscillation would be expected to have undergone two cycles assuming its period is half a Saturn year (14.7 years). This contrast is suggestive that the period of the SSAO is more quasisemiannual.
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Bosh, Amanda Sachie. "Stellar occultation studies of Saturn's rings with the Hubble Space Telescope." Thesis, Massachusetts Institute of Technology, 1994. http://hdl.handle.net/1721.1/35368.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 1994.
Includes bibliographical references (p. 157-162).
by Amanda Sachie Bosh.
Ph.D.
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Books on the topic "Saturn's atmosphere"

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Karmeli͡uk, A. I. Fizicheskie parametry atmosfery Saturna, opredelennye po polose pogloshchenii͡a ammiaka 645.0 HM. Kiev: VINITI, 1990.

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Karmeli︠u︡k, A. I. Fizicheskie parametry atmosfery Saturna, opredelennye po polose pogloshchenii︠a︡ ammiaka 645.0 HM. Kiev: VINITI, 1990.

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Irwin, Patrick. Giant planets of our solar system: Atmospheres, composition, and structure. Chichester, U.K: Springer, 2003.

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Prinn, Ronald G. Khimii͡a︡ i khimicheskai͡a︡ ėvoli͡u︡t͡s︡ii͡a︡ atmosfer Venery, Saturna i Titana po dannym noveĭshikh kosmicheskikh issledovaniĭ: Dvadt͡s︡atʹ pi͡a︡toe chtenie im. V.I. Vernadskogo, 12 marta 1984 goda. Moskva: "Nauka", 1986.

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Bedey, David F. The atmosphere around Saturn's rings: a study of the probability of collision between ring particles and atmospheric molecules. 1986.

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Yung, Yuk L., and William B. DeMore. Photochemistry of Planetary Atmospheres. Oxford University Press, 1999. http://dx.doi.org/10.1093/oso/9780195105018.001.0001.

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Eleven planetary atmospheres are included for detailed study in this reference/text, four for the giant planets (Jupiter, Saturn, Uranus, and Neptune), four for the small bodies (Io, Titan, Triton, and Pluto), and three for the terrestrial planets (Mars, Venus, and Earth). The authors have carried out a comprehensive survey of the principal chemical cycles that control the present composition and past history of planetary atmospheres, using the database provided by recent spacecraft missions supplemented by Earth-based observations.
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J, Gierasch Peter, Leroy Stephen S, and United States. National Aeronautics and Space Administration., eds. Temperature and circulation in the stratospheres of the outer planets. [Washington, DC: National Aeronautics and Space Administration, 1989.

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Irwin, Patrick. Giant Planets of Our Solar System: Atmospheres, Composition, and Structure. Springer, 2010.

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Schrijver, Karel. Habitability of Planets and Moons. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198799894.003.0010.

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The author takes us to visit Saturn’s moon Titan, and Venus, Mars, and to the unconfirmed planet GJ581d. Although we find unearthly conditions on these bodies’ surfaces today, things were different in the past. Even now, there are oceans deep below Titan’s frozen ice shell that itself sees liquid methane rains and vast ethane-filled lakes. Venus and Mars both had liquid water long ago, while Venus may even have been comfortably warm and humid before modern complex life developed on Earth. Many potentially habitable exoplanets are likely locked in their rotation to always face their star with the same side, causing incredible differences between their day and night sides. This chapter reviews how oceans and atmospheres are lost by the Sun’s magnetism or protected by that of the planets’, how masses of carbon dioxide can be stored in solid limestone, and how habitable zones shift to and from planets.
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Infrared spectroscopy of Jupiter and Saturn: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1993.

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Book chapters on the topic "Saturn's atmosphere"

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West, R. A., K. H. Baines, E. Karkoschka, and A. Sánchez-Lavega. "Clouds and Aerosols in Saturn's Atmosphere." In Saturn from Cassini-Huygens, 161–79. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-9217-6_7.

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Nagy, Andrew F., Arvydas J. Kliore, Michael Mendillo, Steve Miller, Luke Moore, Julianne I. Moses, Ingo Müller-Wodarg, and Don Shemansky. "Upper Atmosphere and Ionosphere of Saturn." In Saturn from Cassini-Huygens, 181–201. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-9217-6_8.

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Orton, Glenn S., and Andrew P. Ingersoll. "Saturn's Atmospheric Temperature Structure and Heat Budget." In 1980, Pioneer Saturn, 5871–81. Washington, DC: American Geophysical Union, 2014. http://dx.doi.org/10.1002/9781118782101.ch21.

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Fischer, Georg, Donald A. Gurnett, William S. Kurth, Ferzan Akalin, Philippe Zarka, Ulyana A. Dyudina, William M. Farrell, and Michael L. Kaiser. "Atmospheric Electricity at Saturn." In Space Sciences Series of ISSI, 271–85. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-87664-1_17.

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Genio, Anthony D. Del, Richard K. Achterberg, Kevin H. Baines, F. Michael Flasar, Peter L. Read, Agustín Sánchez-Lavega, and Adam P. Showman. "Saturn Atmospheric Structure and Dynamics." In Saturn from Cassini-Huygens, 113–59. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-9217-6_6.

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Hueso, Ricardo, and Agustín S´nchez-Lavega. "MOIST CONVECTIVE STORMS IN THE ATMOSPHERES OF JUPITER AND SATURN Atmospheric storms in Jupiter and Saturn." In The Many Scales in the Universe, 211–20. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4526-3_18.

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Kliore, Arvydas J., Indu R. Patel, Gunnar F. Lindal, Donald N. Sweetnam, Henry B. Hotz, J. Hunter Waite, and Thomas R. McDonough. "Structure of the Ionosphere and Atmosphere of Saturn from Pioneer 11 Saturn Radio Occultation." In 1980, Pioneer Saturn, 5857–70. Washington, DC: American Geophysical Union, 2014. http://dx.doi.org/10.1002/9781118782101.ch20.

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Owen, Tobias, and Daniel Gautier. "Touring the Saturnian System: The Atmospheres of Titan and Saturn." In The Cassini-Huygens Mission, 347–76. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-3251-2_9.

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Ingersoll, Andrew P. "Titan, Moons, and Small Planets." In Planetary Climates. Princeton University Press, 2013. http://dx.doi.org/10.23943/princeton/9780691145044.003.0006.

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This chapter examines the hydrologic cycle on Saturn's moon Titan, which has an atmosphere of nitrogen and methane. Titan is an evolving atmosphere, close to the lower size limit of objects that can retain a sizeable atmosphere over geologic time. Below this limit, the atmospheres are tenuous and transient. The chapter first provides an overview of Titan's atmospheric evolution before discussing its hydrologic cycle and lakes. It then considers Titan's energetic weather in a low-energy environment, focusing on temperature and winds, and the difficulty of retaining an atmosphere on Titan due to its small gravity and proximity to the Sun. It also explains the anti-greenhouse effect and production of higher hydrocarbons on Titan.
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Sayanagi, Kunio M., Kevin H. Baines, Ulyana Dyudina, Leigh N. Fletcher, Agustín Sánchez-Lavega, and Robert A. West. "Saturn’s Polar Atmosphere." In Saturn in the 21st Century, 337–76. Cambridge University Press, 2018. http://dx.doi.org/10.1017/9781316227220.012.

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Conference papers on the topic "Saturn's atmosphere"

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Andrade, Luis G. "Skimming through Saturn's Atmosphere: The Climax of the Cassini Grand Finale Mission." In 2018 AIAA Guidance, Navigation, and Control Conference. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2018. http://dx.doi.org/10.2514/6.2018-2111.

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Ternovoi, V. Ya. "Experimental Study of Transition of Jupiter and Saturn Atmosphere to Conducting State." In SHOCK COMPRESSION OF CONDENSED MATTER - 2005: Proceedings of the Conference of the American Physical Society Topical Group on Shock Compression of Condensed Matter. AIP, 2006. http://dx.doi.org/10.1063/1.2263607.

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Hewett, Daniel, Brant Billinghurst, Peter Bernath, and Andy Wong. "IDENTIFYING TITAN�S ATMOSPHERE � A LOOK AT HYDROCARBONS POTENTIALLY PRESENT IN THE ATMOSPHERE OF SATURN�S MOST INTERESTING MOON." In 74th International Symposium on Molecular Spectroscopy. Urbana, Illinois: University of Illinois at Urbana-Champaign, 2019. http://dx.doi.org/10.15278/isms.2019.wa04.

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