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  • 1
    Electronic Resource
    Electronic Resource
    Observation of moist convection in Jupiter's atmosphere (2000)
    [s.l.] : Macmillian Magazines Ltd.
    Nature 403 (2000), S. 628-630 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The energy source driving Jupiter's active meteorology is not understood. There are two main candidates: a poorly understood internal heat source and sunlight. Here we report observations of an active storm system possessing both lightning and condensation of water. The storm has a ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/35001017
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  • 2
    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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  • 3
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    Equatorial winds on Saturn and the stratospheric oscillation (2011)
    Springer Nature
    Details
    Publication Date: 2011-11-01
    Description: Equatorial winds on Saturn and the stratospheric oscillation Nature Geoscience 4, 750 (2011). doi:10.1038/ngeo1292 Authors: Liming Li, Xun Jiang, Andrew P. Ingersoll, Anthony D. Del Genio, Carolyn C. Porco, Robert A. West, Ashwin R. Vasavada, Shawn P. Ewald, Barney J. Conrath, Peter J. Gierasch, Amy A. Simon-Miller, Conor A. Nixon, Richard K. Achterberg, Glenn S. Orton, Leigh N. Fletcher & Kevin H. Baines The zonal jets on the giant planets have been thought to be stable in time. A decline in the velocity of Saturn’s equatorial jet has been identified, on the basis of a comparison of cloud-tracking data across two decades, but the differences in cloud speeds have since been suggested to stem from changes in cloud altitude in combination with vertical wind shear, rather than from temporal changes in wind strength at a given height. Here, we combine observations of cloud tracks and of atmospheric temperatures taken by two instruments on the Cassini spacecraft to reveal a significant temporal variation in the strength of the high-altitude equatorial jet on Saturn. Specifically, we find that wind speeds at atmospheric pressure levels of 60 mbar, corresponding to Saturn’s tropopause, increased by about 20 m s−1 between 2004 and 2008, whereas the wind speed has been essentially constant over time in the southern equatorial troposphere. The observations further reveal that the equatorial jet intensified by about 60 m s−1 between 2005 and 2008 in the stratosphere, that is, at pressure levels of 1–5 mbar. Because the wind acceleration is weaker near the tropopause than higher up, in the stratosphere, we conclude that the semi-annual equatorial oscillation of Saturn’s middle atmosphere is also damped as it propagates downwards.
    Print ISSN: 1752-0894
    Electronic ISSN: 1752-0908
    Topics: Geosciences
    Published by Springer Nature
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  • 4
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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
    Details
    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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  • 5
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    The global energy balance of Titan (2011)
    Wiley
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    Publication Date: 2011-12-15
    Description: The global energy budget of planets and their moons is a critical factor to influence the climate change on these objects. Here we report the first measurement of the global emitted power of Titan. Long-term (2004–2010) observations conducted by the Composite Infrared Spectrometer (CIRS) onboard Cassini reveal that the total emitted power by Titan is (2.84 ± 0.01) × 1014 watts. Together with previous measurements of the global absorbed solar power of Titan, the CIRS measurements indicate that the global energy budget of Titan is in equilibrium within measurement error. The uncertainty in the absorbed solar energy places an upper limit on the energy imbalance of 6.0%.
    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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  • 6
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    Depth of a strong jovian jet from a planetary-scale disturbance driven by storms (2008)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2008-01-25
    Description: The atmospheres of the gas giant planets (Jupiter and Saturn) contain jets that dominate the circulation at visible levels. The power source for these jets (solar radiation, internal heat, or both) and their vertical structure below the upper cloud are major open questions in the atmospheric circulation and meteorology of giant planets. Several observations and in situ measurements found intense winds at a depth of 24 bar, and have been interpreted as supporting an internal heat source. This issue remains controversial, in part because of effects from the local meteorology. Here we report observations and modelling of two plumes in Jupiter's atmosphere that erupted at the same latitude as the strongest jet (23 degrees N). The plumes reached a height of 30 km above the surrounding clouds, moved faster than any other feature (169 m s(-1)), and left in their wake a turbulent planetary-scale disturbance containing red aerosols. On the basis of dynamical modelling, we conclude that the data are consistent only with a wind that extends well below the level where solar radiation is deposited.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sanchez-Lavega, A -- Orton, G S -- Hueso, R -- Garcia-Melendo, E -- Perez-Hoyos, S -- Simon-Miller, A -- Rojas, J F -- Gomez, J M -- Yanamandra-Fisher, P -- Fletcher, L -- Joels, J -- Kemerer, J -- Hora, J -- Karkoschka, E -- de Pater, I -- Wong, M H -- Marcus, P S -- Pinilla-Alonso, N -- Carvalho, F -- Go, C -- Parker, D -- Salway, M -- Valimberti, M -- Wesley, A -- Pujic, Z -- England -- Nature. 2008 Jan 24;451(7177):437-40. doi: 10.1038/nature06533.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Departamento de Fisica Aplicada I, ETS Ingenieros, Universidad del Pais Vasco, Alameda Urquijo s/n, 48013 Bilbao, Spain. agustin.sanchez@ehu.es〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18216848" 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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  • 7
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    An equatorial oscillation in Saturn's middle atmosphere (2008)
    Nature Publishing Group (NPG)
    Details
    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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  • 8
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    Polar lightning and decadal-scale cloud variability on Jupiter (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2007-10-13
    Description: Although lightning has been seen on other planets, including Jupiter, polar lightning has been known only on Earth. Optical observations from the New Horizons spacecraft have identified lightning at high latitudes above Jupiter up to 80 degrees N and 74 degrees S. Lightning rates and optical powers were similar at each pole, and the mean optical flux is comparable to that at nonpolar latitudes, which is consistent with the notion that internal heat is the main driver of convection. Both near-infrared and ground-based 5-micrometer thermal imagery reveal that cloud cover has thinned substantially since the 2000 Cassini flyby, particularly in the turbulent wake of the Great Red Spot and in the southern half of the equatorial region, demonstrating that vertical dynamical processes are time-varying on seasonal scales at mid- and low latitudes on Jupiter.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Baines, Kevin H -- Simon-Miller, Amy A -- Orton, Glenn S -- Weaver, Harold A -- Lunsford, Allen -- Momary, Thomas W -- Spencer, John -- Cheng, Andrew F -- Reuter, Dennis C -- Jennings, Donald E -- Gladstone, G R -- Moore, Jeffrey -- Stern, S Alan -- Young, Leslie A -- Throop, Henry -- Yanamandra-Fisher, Padma -- Fisher, Brendan M -- Hora, Joseph -- Ressler, Michael E -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):226-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932285" 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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  • 9
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    Jupiter cloud composition, stratification, convection, and wave motion: a view from new horizons (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2007-10-13
    Description: Several observations of Jupiter's atmosphere made by instruments on the New Horizons spacecraft have implications for the stability and dynamics of Jupiter's weather layer. Mesoscale waves, first seen by Voyager, have been observed at a spatial resolution of 11 to 45 kilometers. These waves have a 300-kilometer wavelength and phase velocities greater than the local zonal flow by 100 meters per second, much higher than predicted by models. Additionally, infrared spectral measurements over five successive Jupiter rotations at spatial resolutions of 200 to 140 kilometers have shown the development of transient ammonia ice clouds (lifetimes of 40 hours or less) in regions of strong atmospheric upwelling. Both of these phenomena serve as probes of atmospheric dynamics below the visible cloud tops.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Reuter, D C -- Simon-Miller, A A -- Lunsford, A -- Baines, K H -- Cheng, A F -- Jennings, D E -- Olkin, C B -- Spencer, J R -- Stern, S A -- Weaver, H A -- Young, L A -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):223-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA. dennis.c.reuter@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932284" target="_blank"〉PubMed〈/a〉
    Keywords: Ammonia ; Atmosphere ; Extraterrestrial Environment ; *Jupiter ; Spacecraft ; 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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  • 10
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    Dynamics of Saturn's south polar vortex (2008)
    American Association for the Advancement of Science (AAAS)
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    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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