Thermal Structure of Jupiter's Upper Atmosphere Derived from the Galileo Probe-Reference-Cited by-同舟云学术

Thermal Structure of Jupiter's Upper Atmosphere Derived from the Galileo Probe

Published:1997-04-04 Issue:5309 Volume:276 Page:102-104
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Seiff Alvin¹,Kirk Donn B.²,Knight Tony C. D.³,Young Leslie A.⁴,Milos Frank S.⁵,Venkatapathy Ethiraj⁶,Mihalov John D.⁷,Blanchard Robert C.⁸,Young Richard E.⁷,Schubert Gerald⁹

Affiliation:

1. Department of Meteorology, San Jose State University Foundation and MS 245-1, Ames Research Center, Moffett Field, CA 94035, USA.

2. University of Oregon, 37465 Riverside Drive, Pleasant Hill, Oregon 97455, USA.

3. 2370 S. Brentwood St., Lakewood, CO 80227, USA.

4. Center for Space Physics, Boston University, 725 Commonwealth Ave., Boston, Massachusetts 02215, USA.

5. M.S 234-1, Ames Research Center, NASA, Moffett Field, CA 94035, USA.

6. Eloret Institute, MS 230-2, Ames Research Center, Moffett Field, CA 94035, USA.

7. MS 245-3, Ames Research Center, Moffett Field, CA 94035, USA.

8. MS 408A, Langley Research Center, NASA, Hampton, VA 23681, USA.

9. Department of Earth and Space Sciences, University of California, Los Angeles, CA 90024, USA.

Abstract

Temperatures in Jupiter's atmosphere derived from Galileo Probe deceleration data increase from 109 kelvin at the 175-millibar level to 900 ± 40 kelvin at 1 nanobar, consistent with Voyager remote sensing data. Wavelike oscillations are present at all levels. Vertical wavelengths are 10 to 25 kilometers in the deep isothermal layer, which extends from 12 to 0.003 millibars. Above the 0.003-millibar level, only 90- to 270- kilometer vertical wavelengths survive, suggesting dissipation of wave energy as the probable source of upper atmosphere heating.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

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