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  • 1
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    A Numerical Technique for Two Way Radio Occultations by Oblate Axisymmetric Atmospheres with Zonal Winds (2015)
    Wiley
    Details
    Publication Date: 2015-06-28
    Description: The Ultra Stable Oscillator aboard the Cassini spacecraft failed in late 2011, which means that all radio occultations after that date have to be done in two way mode, using a ground based signal transmitted to the spacecraft as the frequency reference. Here we present the numerical technique we use to analyze the data from the two way atmospheric radio occultations of both Saturn and Titan that have occured since the USO failure, along with the theoretical reasons behind this technique. Since our two way technique is based upon our earlier one way technique which used the USO as the frequency reference, we also present our one way technique which we used for Saturn occultations prior to the loss of the USO.
    Print ISSN: 0048-6604
    Electronic ISSN: 1944-799X
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Saturn's equatorial oscillation: Evidence of descending thermal structure from Cassini radio occultations (2011)
    Wiley
    Details
    Publication Date: 2011-04-28
    Description: A series of near-equatorial radio occultations of Cassini by Saturn occurred in 2005 and again in 2009–2010. Comparison of the temperature-pressure profiles obtained from the two sets of occultations shows evidence of a descending pattern in the stratosphere that is similar to those associated with equatorial oscillations in Earth's middle atmosphere. This is the first time that this descent has been observed in another planetary atmosphere. If absorption of upwardly propagating waves drives the descent, the implied absorbed flux is 0.05 m2 s−2, at least as large if not greater than on Earth.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    Evolution of the equatorial oscillation in Saturn's stratosphere between 2005 and 2010 from Cassini/CIRS limb data analysis (2011)
    Wiley
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    Publication Date: 2011-05-04
    Description: We present an analysis of thermal infrared spectra acquired in limb viewing geometry by Cassini/CIRS in February 2010. We retrieve vertical profiles of Saturn's stratospheric temperature from 20 hPa to 10−2 hPa, at 9 latitudes between 20°N and 20°S. Using the gradient thermal wind equation, we derive a map of the zonal wind field. Both the temperature and the zonal wind vertical profiles exhibit an oscillation in the equatorial region. These results are compared to the temperature and zonal wind maps obtained from 2005–2006 CIRS limb data, when this oscillation was first reported. In both epochs, strong temperature anomalies at the equator (up to 20K) are consistent with adiabatic heating (cooling) due to a sinking (rising) motion at a speed of 0.1–0.2 mm/s. Finally, we show that the altitude of the maximum eastward wind has moved downwards by 1.3 scale heights in 4.2 years, hence with a ‘phase’ speed of ∼0.5 mm/s. This rate is consistent with the estimated period of 14.7 years for the equatorial oscillation, and requires a local zonal acceleration of 1.1 × 10−6 m.s−2 at the 2.5 hPa pressure level. This downward propagation of the oscillation is consistent with it being driven by absorption of upwardly propagating waves.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 4
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    An equatorial oscillation in Saturn's middle atmosphere (2008)
    Nature Publishing Group (NPG)
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    Publication Date: 2008-05-10
    Description: The middle atmospheres of planets are driven by a combination of radiative heating and cooling, mean meridional motions, and vertically propagating waves (which originate in the deep troposphere). It is very difficult to model these effects and, therefore, observations are essential to advancing our understanding of atmospheres. The equatorial stratospheres of Earth and Jupiter oscillate quasi-periodically on timescales of about two and four years, respectively, driven by wave-induced momentum transport. On Venus and Titan, waves originating from surface-atmosphere interaction and inertial instability are thought to drive the atmosphere to rotate more rapidly than the surface (superrotation). However, the relevant wave modes have not yet been precisely identified. Here we report infrared observations showing that Saturn has an equatorial oscillation like those found on Earth and Jupiter, as well as a mid-latitude subsidence that may be associated with the equatorial motion. The latitudinal extent of Saturn's oscillation shows that it obeys the same basic physics as do those on Earth and Jupiter. Future highly resolved observations of the temperature profile together with modelling of these three different atmospheres will allow us determine the wave mode, the wavelength and the wave amplitude that lead to middle atmosphere oscillation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fouchet, T -- Guerlet, S -- Strobel, D F -- Simon-Miller, A A -- Bezard, B -- Flasar, F M -- England -- Nature. 2008 May 8;453(7192):200-2. doi: 10.1038/nature06912.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉LESIA, Observatoire de Paris, Universite Pierre et Marie Curie, CNRS, Paris 7, Meudon F-92195, France. thierry.fouchet@obspm.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18464737" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 5
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    Planetary science. Titan's polar weather (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-09-16
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flasar, F M -- New York, N.Y. -- Science. 2006 Sep 15;313(5793):1582-3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Systems Laboratory, NASA Goddard Spaceflight Center, Greenbelt, MD 20771, USA. f.m.flasar@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16973865" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Cold Temperature ; *Ethane ; Extraterrestrial Environment ; Gases ; Organic Chemicals ; *Saturn
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    Dynamics of Saturn's south polar vortex (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-03-29
    Description: The camera onboard the Cassini spacecraft has allowed us to observe many of Saturn's cloud features. We present observations of Saturn's south polar vortex (SPV) showing that it shares some properties with terrestrial hurricanes: cyclonic circulation, warm central region (the eye) surrounded by a ring of high clouds (the eye wall), and convective clouds outside the eye. The polar location and the absence of an ocean are major differences. It also shares properties with the polar vortices on Venus, such as polar location, cyclonic circulation, warm center, and long lifetime, but the Venus vortices have cold collars and are not associated with convective clouds. The SPV's combination of properties is unique among vortices in the solar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Dyudina, Ulyana A -- Ingersoll, Andrew P -- Ewald, Shawn P -- Vasavada, Ashwin R -- West, Robert A -- Del Genio, Anthony D -- Barbara, John M -- Porco, Carolyn C -- Achterberg, Richard K -- Flasar, F Michael -- Simon-Miller, Amy A -- Fletcher, Leigh N -- New York, N.Y. -- Science. 2008 Mar 28;319(5871):1801. doi: 10.1126/science.1153633.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. ulyana@gps.caltech.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18369142" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 7
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    Temperature and composition of Saturn's polar hot spots and hexagon (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-01-05
    Description: Saturn's poles exhibit an unexpected symmetry in hot, cyclonic polar vortices, despite huge seasonal differences in solar flux. The cores of both vortices are depleted in phosphine gas, probably resulting from subsidence of air into the troposphere. The warm cores are present throughout the upper troposphere and stratosphere at both poles. The thermal structure associated with the marked hexagonal polar jet at 77 degrees N has been observed for the first time. Both the warm cyclonic belt at 79 degrees N and the cold anticyclonic zone at 75 degrees N exhibit the hexagonal structure.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fletcher, L N -- Irwin, P G J -- Orton, G S -- Teanby, N A -- Achterberg, R K -- Bjoraker, G L -- Read, P L -- Simon-Miller, A A -- Howett, C -- de Kok, R -- Bowles, N -- Calcutt, S B -- Hesman, B -- Flasar, F M -- New York, N.Y. -- Science. 2008 Jan 4;319(5859):79-81. doi: 10.1126/science.1149514.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Atmospheric, Oceanic, and Planetary Physics, Department of Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford OX1 3PU, UK. fletcher@atm.ox.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18174438" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    Thermal structure and dynamics of Saturn's northern springtime disturbance (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-05-21
    Description: Saturn's slow seasonal evolution was disrupted in 2010-2011 by the eruption of a bright storm in its northern spring hemisphere. Thermal infrared spectroscopy showed that within a month, the resulting planetary-scale disturbance had generated intense perturbations of atmospheric temperatures, winds, and composition between 20 degrees and 50 degrees N over an entire hemisphere (140,000 kilometers). The tropospheric storm cell produced effects that penetrated hundreds of kilometers into Saturn's stratosphere (to the 1-millibar region). Stratospheric subsidence at the edges of the disturbance produced "beacons" of infrared emission and longitudinal temperature contrasts of 16 kelvin. The disturbance substantially altered atmospheric circulation, transporting material vertically over great distances, modifying stratospheric zonal jets, exciting wave activity and turbulence, and generating a new cold anticyclonic oval in the center of the disturbance at 41 degrees N.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fletcher, Leigh N -- Hesman, Brigette E -- Irwin, Patrick G J -- Baines, Kevin H -- Momary, Thomas W -- Sanchez-Lavega, Agustin -- Flasar, F Michael -- Read, Peter L -- Orton, Glenn S -- Simon-Miller, Amy -- Hueso, Ricardo -- Bjoraker, Gordon L -- Mamoutkine, Andrei -- del Rio-Gaztelurrutia, Teresa -- Gomez, Jose M -- Buratti, Bonnie -- Clark, Roger N -- Nicholson, Philip D -- Sotin, Christophe -- New York, N.Y. -- Science. 2011 Jun 17;332(6036):1413-7. doi: 10.1126/science.1204774. Epub 2011 May 19.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Atmospheric, Oceanic and Planetary Physics, Department of Physics, Clarendon Laboratory, University of Oxford, Parks Road, Oxford, OX1 3PU, UK. fletcher@atm.ox.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21596955" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 9
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    The ionosphere of Europa from Galileo radio occultations (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1997-07-18
    Description: The Galileo spacecraft performed six radio occultation observations of Jupiter's Galilean satellite Europa during its tour of the jovian system. In five of the six instances, these occultations revealed the presence of a tenuous ionosphere on Europa, with an average maximum electron density of nearly 10(4) per cubic centimeter near the surface and a plasma scale height of about 240 +/- 40 kilometers from the surface to 300 kilometers and of 440 +/- 60 kilometers above 300 kilometers. Such an ionosphere could be produced by solar photoionization and jovian magnetospheric particle impact in an atmosphere having a surface density of about 10(8) electrons per cubic centimeter. If this atmosphere is composed primarily of O2, then the principal ion is O2+ and the neutral atmosphere temperature implied by the 240-kilometer scale height is about 600 kelvin. If it is composed of H2O, the principal ion is H3O+ and the neutral temperature is about 340 kelvin. In either case, these temperatures are much higher than those observed on Europa's surface, and an external heating source from the jovian magnetosphere is required.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kliore, A J -- Hinson, D P -- Flasar, F M -- Nagy, A F -- Cravens, T E -- New York, N.Y. -- Science. 1997 Jul 18;277(5324):355-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9219689" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment ; *Hydrogen ; *Jupiter ; Magnetics ; *Oxygen ; Temperature ; *Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
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    Titan's atmospheric temperatures, winds, and composition (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-05-17
    Description: Temperatures obtained from early Cassini infrared observations of Titan show a stratopause at an altitude of 310 kilometers (and 186 kelvin at 15 degrees S). Stratospheric temperatures are coldest in the winter northern hemisphere, with zonal winds reaching 160 meters per second. The concentrations of several stratospheric organic compounds are enhanced at mid- and high northern latitudes, and the strong zonal winds may inhibit mixing between these latitudes and the rest of Titan. Above the south pole, temperatures in the stratosphere are 4 to 5 kelvin cooler than at the equator. The stratospheric mole fractions of methane and carbon monoxide are (1.6 +/- 0.5) x 10(-2) and (4.5 +/- 1.5) x 10(-5), respectively.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flasar, F M -- Achterberg, R K -- Conrath, B J -- Gierasch, P J -- Kunde, V G -- Nixon, C A -- Bjoraker, G L -- Jennings, D E -- Romani, P N -- Simon-Miller, A A -- Bezard, B -- Coustenis, A -- Irwin, P G J -- Teanby, N A -- Brasunas, J -- Pearl, J C -- Segura, M E -- Carlson, R C -- Mamoutkine, A -- Schinder, P J -- Barucci, A -- Courtin, R -- Fouchet, T -- Gautier, D -- Lellouch, E -- Marten, A -- Prange, R -- Vinatier, S -- Strobel, D F -- Calcutt, S B -- Read, P L -- Taylor, F W -- Bowles, N -- Samuelson, R E -- Orton, G S -- Spilker, L J -- Owen, T C -- Spencer, J R -- Showalter, M R -- Ferrari, C -- Abbas, M M -- Raulin, F -- Edgington, S -- Ade, P -- Wishnow, E H -- New York, N.Y. -- Science. 2005 May 13;308(5724):975-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15894528" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Carbon Monoxide ; Extraterrestrial Environment ; *Hydrocarbons ; *Methane ; *Nitriles ; *Saturn ; Spacecraft ; Temperature ; Wind
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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