Jupiter's thermosphere general circulation model: thermal and dynamical structures

Details Jupiter's thermosphere general circulation model: thermal and dynamical structures Jupiter's thermosphere general circulation model: thermal and dynamical structures

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....6767m&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #6767

Computer Science

Scientific paper

Recent observations of infrared and FUV auroral emissions from Jupiter have shown the presence of high-speed (>~2km/s) winds in the jovian thermosphere. The neutral atmospheric structure measured in-situ by the Galileo probe near the jovian equator exhibited wave-like oscillations in the temperature profile at altitudes of 133--1029~km. The derived exospheric temperature was ˜940~K. While no in-situ measurement is available for the neutral atmosphere of Jupiter's auroral region, infrared and ultraviolet spectrographic imaging results indicate auroral exospheric temperatures >1200~K. We examine this hypothesis using a fully 3-D JTGCM that has been developed and exercised to address global scale temperature, wind, and neutral-ion specie distributions. It was developed from a suitable adaptation of the NCAR Thermosphere Ionosphere General Circulation Model (TIGCM). An ion drag scheme was incorporated. A convection electric field was estimated and corresponding ion drifts were generated. These prescriptions provide a means to test the general impact of ion drag and Joule heating on the JTGCM neutral winds. The JTGCM has been fully spun-up and exercised for various cases to simulate 3-component neutral winds, and corresponding temperature and density distributions. The horizontal winds at the ionospheric heights vary from 0.5 km/s to 1.6 km/s and auroral temperatures from 1000 K to 3800 K depending on the magnitude of Joule heating. The equatorial temperature profiles from the JTGCM are compared with the measured temperature structure from the Galileo ASI data. The best fit to the data implies that the major energy source for heating the equatorial atmosphere is due to adiabatic heating induced by the downward motion of the neutral atmosphere. Further details of the JTGCM code and results for moderately strong auroral heating, ion drag, and ion drag plus Joule heating will be presented.

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