排序方式: 共有5条查询结果,搜索用时 156 毫秒
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Orton GS Yanamandra-Fisher PA Fisher BM Friedson AJ Parrish PD Nelson JF Bauermeister AS Fletcher L Gezari DY Varosi F Tokunaga AT Caldwell J Baines KH Hora JL Ressler ME Fujiyoshi T Fuse T Hagopian H Martin TZ Bergstralh JT Howett C Hoffmann WF Deutsch LK Van Cleve JE Noe E Adams JD Kassis M Tollestrup E 《Nature》2008,453(7192):196-199
Observations of oscillations of temperature and wind in planetary atmospheres provide a means of generalizing models for atmospheric dynamics in a diverse set of planets in the Solar System and elsewhere. An equatorial oscillation similar to one in the Earth's atmosphere has been discovered in Jupiter. Here we report the existence of similar oscillations in Saturn's atmosphere, from an analysis of over two decades of spatially resolved observations of its 7.8-microm methane and 12.2-microm ethane stratospheric emissions, where we compare zonal-mean stratospheric brightness temperatures at planetographic latitudes of 3.6 degrees and 15.5 degrees in both the northern and the southern hemispheres. These results support the interpretation of vertical and meridional variability of temperatures in Saturn's stratosphere as a manifestation of a wave phenomenon similar to that on the Earth and in Jupiter. The period of this oscillation is 14.8 +/- 1.2 terrestrial years, roughly half of Saturn's year, suggesting the influence of seasonal forcing, as is the case with the Earth's semi-annual oscillation. 相似文献
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Sánchez-Lavega A Orton GS Hueso R García-Melendo E Pérez-Hoyos S Simon-Miller A Rojas JF Gómez JM Yanamandra-Fisher P Fletcher L Joels J Kemerer J Hora J Karkoschka E de Pater I Wong MH Marcus PS Pinilla-Alonso N Carvalho F Go C Parker D Salway M Valimberti M Wesley A Pujic Z 《Nature》2008,451(7177):437-440
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. 相似文献
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An intense stratospheric jet on Jupiter 总被引:1,自引:0,他引:1
Flasar FM Kunde VG Achterberg RK Conrath BJ Simon-Miller AA Nixon CA Gierasch PJ Romani PN Bézard B Irwin P Bjoraker GL Brasunas JC Jennings DE Pearl JC Smith MD Orton GS Spilker LJ Carlson R Calcutt SB Read PL Taylor FW Parrish P Barucci A Courtin R Coustenis A Gautier D Lellouch E Marten A Prangé R Biraud Y Fouchet T Ferrari C Owen TC Abbas MM Samuelson RE Raulin F Ade P Césarsky CJ Grossman KU Coradini A 《Nature》2004,427(6970):132-135
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 high-latitude stratosphere and weather in the lower atmosphere. Ground-based observations have suggested that similar temperature oscillations (with a 4-5-yr cycle) occur on Jupiter, but these data suffer from poor vertical resolution and Jupiter's stratospheric wind velocities have not yet been determined. Here we report maps of temperatures and winds with high spatial resolution, obtained from spacecraft measurements of infrared spectra of Jupiter's stratosphere. We find an intense, high-altitude equatorial jet with a speed of approximately 140 m s(-1), whose spatial structure resembles that of a quasi-quadrennial oscillation. Wave activity in the stratosphere also appears analogous to that occurring on Earth. A strong interaction between Jupiter and its plasma environment produces hot spots in its upper atmosphere and stratosphere near its poles, and the temperature maps define the penetration of the hot spots into the stratosphere. 相似文献
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