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

• Published in: Science (American Association for the Advancement of Science) 1997-04, Vol.276 (5309), p.102-104
• Main Authors: Seiff, Alvin, Kirk, Donn B., Tony C. D. Knight, Young, Leslie A., Milos, Frank S., Venkatapathy, Ethiraj, Mihalov, John D., Blanchard, Robert C., Young, Richard E., Schubert, Gerald
• Format: Article
• Language: English
• Subjects: Acceleration; Altitude; Astronomy; Atmosphere; Average linear density; Climate; Density; Earth, ocean, space; Exact sciences and technology; Heat; Jovian atmosphere; Jupiter; Jupiter (Planet); Measurement Techniques; Motion; Neutral atmospheres; Occultation; Planetary atmospheres; Planetary probes; Planetary, asteroid, and satellite characteristics and properties; Planets; Planets, their satellites and rings. Asteroids; Profiles; Scientific Concepts; Solar system; Spacecraft; Temperature; Tropopause; Upper atmosphere; Wavelengths
• ISSN: 0036-8075; 1095-9203
• DOI: 10.1126/science.276.5309.102

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.