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  • 1
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    Seasonal evolution of Titan's stratosphere during the Cassini mission (2019)
    Wiley
    Details
    Publication Date: 2019
    Description: Abstract Titan's stratosphere exhibits significant seasonal changes, including break‐up and formation of polar vortices. Here we present the first analysis of mid‐infrared mapping observations from Cassini's Composite InfraRed Spectrometer (CIRS) to cover the entire mission (Ls=293‐93°, 2004‐‐2017)‐mid‐northern winter to northern summer solstice. The north‐polar winter vortex persisted well after equinox, starting break‐up around Ls~60°, and fully dissipating by Ls~90°.Absence of enriched polar air spreading to lower latitudes suggests large‐scale circulation changes and photochemistry control chemical evolution during vortex break‐up. South‐polar vortex formation commenced soon after equinox and by Ls~60° was more enriched in trace gases than the northern mid‐winter vortex and had temperatures ~20 K colder. This suggests early‐winter and mid‐winter vortices are dominated by different processes ‐‐ radiative cooling and subsidence‐induced adiabatic heating respectively. By the end of the mission Ls93° south‐polar conditions were approaching those observed in the north at Ls=293°, implying seasonal symmetry in Titan's vortices.
    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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  • 2
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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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  • 3
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    Temperatures, winds, and composition in the saturnian system (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-12-25
    Description: Stratospheric temperatures on Saturn imply a strong decay of the equatorial winds with altitude. If the decrease in winds reported from recent Hubble Space Telescope images is not a temporal change, then the features tracked must have been at least 130 kilometers higher than in earlier studies. Saturn's south polar stratosphere is warmer than predicted from simple radiative models. The C/H ratio on Saturn is seven times solar, twice Jupiter's. Saturn's ring temperatures have radial variations down to the smallest scale resolved (100 kilometers). Diurnal surface temperature variations on Phoebe suggest a more porous regolith than on the jovian satellites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flasar, F M -- Achterberg, R K -- Conrath, B J -- Pearl, J C -- Bjoraker, G L -- Jennings, D E -- Romani, P N -- Simon-Miller, A A -- Kunde, V G -- Nixon, C A -- Bezard, B -- Orton, G S -- Spilker, L J -- Spencer, J R -- Irwin, P G J -- Teanby, N A -- Owen, T C -- Brasunas, J -- Segura, M E -- Carlson, R C -- Mamoutkine, A -- Gierasch, P J -- Schinder, P J -- Showalter, M R -- Ferrari, C -- Barucci, A -- Courtin, R -- Coustenis, A -- Fouchet, T -- Gautier, D -- Lellouch, E -- Marten, A -- Prange, R -- Strobel, D F -- Calcutt, S B -- Read, P L -- Taylor, F W -- Bowles, N -- Samuelson, R E -- Abbas, M M -- Raulin, F -- Ade, P -- Edgington, S -- Pilorz, S -- Wallis, B -- Wishnow, E H -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1247-51. Epub 2004 Dec 23.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Aeronautics and Space Administration (NASA)/Goddard Space Flight Center, Code 693, 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/15618486" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Carbon ; Extraterrestrial Environment ; Hydrogen ; Methane ; *Saturn ; Spacecraft ; Spectrum Analysis ; 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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  • 4
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    Jupiter's atmospheric composition from the Cassini thermal infrared spectroscopy experiment (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-21
    Description: The Composite Infrared Spectrometer observed Jupiter in the thermal infrared during the swing-by of the Cassini spacecraft. Results include the detection of two new stratospheric species, the methyl radical and diacetylene, gaseous species present in the north and south auroral infrared hot spots; determination of the variations with latitude of acetylene and ethane, the latter a tracer of atmospheric motion; observations of unexpected spatial distributions of carbon dioxide and hydrogen cyanide, both considered to be products of comet Shoemaker-Levy 9 impacts; characterization of the morphology of the auroral infrared hot spot acetylene emission; and a new evaluation of the energetics of the northern auroral infrared hot spot.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kunde, V G -- Flasar, F M -- Jennings, D E -- Bezard, B -- Strobel, D F -- Conrath, B J -- Nixon, C A -- Bjoraker, G L -- Romani, P N -- Achterberg, R K -- Simon-Miller, A A -- Irwin, P -- Brasunas, J C -- Pearl, J C -- Smith, M D -- Orton, G S -- Gierasch, P J -- Spilker, L J -- Carlson, R C -- Mamoutkine, A A -- Calcutt, S B -- Read, P L -- Taylor, F W -- Fouchet, T -- Parrish, P -- Barucci, A -- Courtin, R -- Coustenis, A -- Gautier, D -- Lellouch, E -- Marten, A -- Prange, R -- Biraud, Y -- Ferrari, C -- Owen, T C -- Abbas, M M -- Samuelson, R E -- Raulin, F -- Ade, P -- Cesarsky, C J -- Grossman, K U -- Coradini, A -- New York, N.Y. -- Science. 2004 Sep 10;305(5690):1582-6. Epub 2004 Aug 19.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Maryland, College Park, MD 20742, USA. Virgil.G.Kunde.1@gsfc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15319491" target="_blank"〉PubMed〈/a〉
    Keywords: Acetylene ; Atmosphere ; *Carbon Dioxide ; Ethane ; Extraterrestrial Environment ; *Hydrocarbons ; *Hydrogen Cyanide ; *Jupiter ; Spacecraft ; Spectrum Analysis ; Temperature
    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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  • 5
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    Active upper-atmosphere chemistry and dynamics from polar circulation reversal on Titan (2012)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2012-11-30
    Description: Saturn's moon Titan has a nitrogen atmosphere comparable to Earth's, with a surface pressure of 1.4 bar. Numerical models reproduce the tropospheric conditions very well but have trouble explaining the observed middle-atmosphere temperatures, composition and winds. The top of the middle-atmosphere circulation has been thought to lie at an altitude of 450 to 500 kilometres, where there is a layer of haze that appears to be separated from the main haze deck. This 'detached' haze was previously explained as being due to the co-location of peak haze production and the limit of dynamical transport by the circulation's upper branch. Here we report a build-up of trace gases over the south pole approximately two years after observing the 2009 post-equinox circulation reversal, from which we conclude that middle-atmosphere circulation must extend to an altitude of at least 600 kilometres. The primary drivers of this circulation are summer-hemisphere heating of haze by absorption of solar radiation and winter-hemisphere cooling due to infrared emission by haze and trace gases; our results therefore imply that these effects are important well into the thermosphere (altitudes higher than 500 kilometres). This requires both active upper-atmosphere chemistry, consistent with the detection of high-complexity molecules and ions at altitudes greater than 950 kilometres, and an alternative explanation for the detached haze, such as a transition in haze particle growth from monomers to fractal structures.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Teanby, Nicholas A -- Irwin, Patrick G J -- Nixon, Conor A -- de Kok, Remco -- Vinatier, Sandrine -- Coustenis, Athena -- Sefton-Nash, Elliot -- Calcutt, Simon B -- Flasar, F Michael -- England -- Nature. 2012 Nov 29;491(7426):732-5. doi: 10.1038/nature11611.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉School of Earth Sciences, University of Bristol, Wills Memorial Building, Queen's Road, Bristol BS8 1RJ, UK. n.teanby@bristol.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23192150" 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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  • 6
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    ALMA detection and astrobiological potential of vinyl cyanide on Titan (2017)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2017-07-29
    Description: Recent simulations have indicated that vinyl cyanide is the best candidate molecule for the formation of cell membranes/vesicle structures in Titan’s hydrocarbon-rich lakes and seas. Although the existence of vinyl cyanide (C 2 H 3 CN) on Titan was previously inferred using Cassini mass spectrometry, a definitive detection has been lacking until now. We report the first spectroscopic detection of vinyl cyanide in Titan’s atmosphere, obtained using archival data from the Atacama Large Millimeter/submillimeter Array (ALMA), collected from February to May 2014. We detect the three strongest rotational lines of C 2 H 3 CN in the frequency range of 230 to 232 GHz, each with 〉4 confidence. Radiative transfer modeling suggests that most of the C 2 H 3 CN emission originates at altitudes of 200 km, in agreement with recent photochemical models. The vertical column densities implied by our best-fitting models lie in the range of 3.7 x 10 13 to 1.4 x 10 14 cm –2 . The corresponding production rate of vinyl cyanide and its saturation mole fraction imply the availability of sufficient dissolved material to form ~10 7 cell membranes/cm 3 in Titan’s sea Ligeia Mare.
    Electronic ISSN: 2375-2548
    Topics: Natural Sciences in General
    Published by American Association for the Advancement of Science (AAAS)
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  • 7
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    Less absorbed solar energy and more internal heat for Jupiter (2018)
    Springer Nature
    Details
    Publication Date: 2018-09-14
    Description: Less absorbed solar energy and more internal heat for Jupiter Less absorbed solar energy and more internal heat for Jupiter, Published online: 13 September 2018; doi:10.1038/s41467-018-06107-2 Radiant energy budgets and internal heat play a key role in the evolution of planets. Here, the authors analyze data from the Cassini mission to show that Jupiter’s radiant energy and internal heat budgets are significantly larger than previous estimates.
    Electronic ISSN: 2041-1723
    Topics: Biology , Chemistry and Pharmacology , Natural Sciences in General , Physics
    Published by Springer Nature
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  • 8
    Electronic Resource
    Electronic Resource
    An intense stratospheric jet on Jupiter (2004)
    [s.l.] : Macmillian Magazines Ltd.
    Nature 427 (2004), S. 132-135 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The Earth's equatorial stratosphere shows oscillations in which the east–west winds reverse direction and the temperatures change cyclically with a period of about two years. This phenomenon, called the quasi-biennial oscillation, also affects the dynamics of the mid- and ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/nature02142
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  • 9
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    Black holes in stellar-mass binary systems: expiating original spin? (2016)
    Oxford University Press
    Details
    Publication Date: 2016-08-04
    Description: We investigate systematically whether accreting black hole systems are likely to reach global alignment of the black hole spin and its accretion disc with the binary plane. In low-mass X-ray binaries (LMXBs), there is only a modest tendency to reach such global alignment, and it is difficult to achieve fully: except for special initial conditions, we expect misalignment of the spin and orbital planes by ~1 rad for most of the LMXB lifetime. The same is expected in high-mass X-ray binaries. A fairly close approach to global alignment is likely in most stellar-mass ultraluminous X-ray binary systems (ULXs) where the companion star fills its Roche lobe and transfers mass on a thermal or nuclear time-scale to a black hole of lower mass. These systems are unlikely to show orbital eclipses, as their emission cones are close to the hole's spin axis. This offers a potential observational test, as models for ULXs invoking intermediate-mass black holes do predict eclipses for ensembles of 10 systems. Recent observational work shows that eclipses are either absent or extremely rare in ULXs, supporting the picture that most ULXs are stellar-mass binaries with companion stars more massive than the accretor.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    AGN flickering and chaotic accretion (2015)
    Oxford University Press
    Details
    Publication Date: 2015-08-19
    Description: Observational arguments suggest that the growth phases of the supermassive black holes in active galactic nuclei have a characteristic time-scale ~10 5  yr. We show that this is the time-scale expected in the chaotic accretion picture of black hole feeding, because of the effect of self-gravity in limiting the mass of any accretion-disc feeding event.
    Print ISSN: 1745-3925
    Electronic ISSN: 1745-3933
    Topics: Physics
    Published by Oxford University Press
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