Reconciling Galileo Probe Data and Ground-Based Radio Observations of Ammonia on Jupiter

Details Reconciling Galileo Probe Data and Ground-Based Radio Observations of Ammonia on Jupiter Reconciling Galileo Probe Data and Ground-Based Radio Observations of Ammonia on Jupiter

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icar..149...66d&link_type=abstract

Icarus, Volume 149, Issue 1, pp. 66-78 (2001).

Physics

27

Scientific paper

Prior to the Galileo probe entry in Jupiter's atmosphere, the ammonia abundance in the planet's deep atmosphere as deduced from microwave observations was thought to be close to the solar N value at P>3 bar and subsolar at P<2 bar. Analysis of the attenuation of the probe radio signal during its descent in Jupiter's atmosphere suggested NH3 to be 3.6+/-0.5 times solar N at P>8 bar (Folkner et al. 1998). Assuming this high value is globally representative of the NH3 abundance in Jupiter's deep atmosphere, we show in this article that to match Jupiter's microwave spectrum the ammonia abundance must, globally, decrease at pressures P<~4 bar, and reach subsolar (<~0.5) values at P<~2 bar. We confirm earlier analysis of the 1.3-cm wavelength region indicating that the disk-averaged relative humidity must be of the order of 10% at P<0.55 bar. We discuss various ways in which NH3 could decrease globally at altitudes well below the level where the NH3-ice clouds form. We also present radio images of Jupiter taken with the VLA at 2, 3.6, and 6 cm wavelength in November/December 1995 and January 1996. The Galileo probe entered Jupiter's atmosphere on 7 December 1995, at a latitude of 6.5°N, i.e., at the southern edge of the north equatorial belt (NEB). Simulations of our data suggest that the longitude-averaged NH3 abundance in the NEB at the time of the Galileo probe entry is of the order of 50-70% of the value in the equatorial zone (EZ), while the NH3 abundance in the EZ is about <~0.5×solar N. This low ammonia abundance in the NEB must extend down to the ~4- to 6-bar level.

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