Depth of a strong jovian jet from a planetary-scale disturbance driven by storms

被引：80

作者：

Sanchez-Lavega, A. ^{[1
]}

Orton, G. S. ^{[2
]}

Hueso, R. ^{[1
]}

Garcia-Melendo, E. ^{[3
]}

Perez-Hoyos, S. ^{[1
]}

Simon-Miller, A. ^{[4
]}

Rojas, J. F. ^{[5
]}

Gomez, J. M. ^{[3
]}

Yanamandra-Fisher, P. ^{[2
]}

Fletcher, L. ^{[6
]}

Joels, J. ^{[7
]}

Kemerer, J. ^{[8
]}

Hora, J. ^{[9
]}

Karkoschka, E. ^{[10
]}

de Pater, I. ^{[11
]}

Wong, M. H. ^{[11
]}

Marcus, P. S. ^{[12
]}

Pinilla-Alonso, N. ^{[13
]}

Carvalho, F. ^{[14
]}

Go, C. ^{[15
]}

Parker, D. ^{[16
]}

Salway, M. ^{[17
]}

Valimberti, M. ^{[18
]}

Wesley, A. ^{[19
]}

Pujic, Z.

机构：

[1] Univ Basque Country, ETS Ingenieros, Dept Fis Aplicada 1, Bilbao 48013, Spain

[2] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[3] Esteve Duran Observ Fdn, Seva 085330, Spain

[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[5] Univ Basque Country, EUITI, Dept Fis Aplicada 1, Bilbao 48013, Spain

[6] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England

[7] Principia Coll, Elsah, IL 62028 USA

[8] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA

[9] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[10] Univ Arizona, Tucson, AZ 85721 USA

[11] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[12] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA

[13] Telescopio Nazl Galileo Galilei, Santa Cruz De La Palma 38700, Spain

[14] Ctr Estudos Universo, BR-17380000 Brotas, Brazil

[15] Univ San Carlos, Dept Phys, Cebu 6000, Philippines

[16] Assoc Lunar & Planetary Observers, Coral Gables, FL 33156 USA

[17] IcelnSpace, Wyoming, NSW 2250, Australia

[18] Astron Soc Victoria, Melbourne, Vic 3001, Australia

[19] Math & Comp Sci, Murrumbateman 2582, Australia

来源：

NATURE | 2008年 / 451卷 / 7177期

基金：

美国国家科学基金会;

关键词：

D O I：

10.1038/nature06533

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

The atmospheres of the gas giant planets ( Jupiter and Saturn) contain jets that dominate the circulation at visible levels(1,2). 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(1-3). Several observations(1) and in situ measurements(4) found intense winds at a depth of 24 bar, and have been interpreted as supporting an internal heat source. This issue remains controversial(5), in part because of effects from the local meteorology(6). 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.

引用

页码：437 / 440

页数：4

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