Radiative Balance and Dynamics in the Stratosphere of Jupiter: Results from a Latitude-Dependent Aerosol Heating Model

Structure of the Jovian Stratosphere at the Galileo Probe Entry Site

“…Moreno and Sedeno (1997) followed earlier authors in assuming the distributions of C 2 H 2 and C 2 H 6 to be uniform with latitude and altitude. Moreno and Sedano (1997) found good agreement with West et al (1992) at pressures greater than 100 mbar but a significantly different circulation pattern at lower pressures, as a consequence of the different aerosol heating pattern.…”

“…These data provide higher spatial resolution than possible with the IUE and Voyager data and the aerosol distribution derived by Moreno and Sedano (1997) has fewer aerosols and therefore less heating than that of West et al (1992) at high northern latitudes. The treatment of gaseous opacities was similar in Moreno and Sedano (1997) and West et al (1992), with the exception that the former authors included radiative cooling by NH 3 , which was neglected in earlier studies. Moreno and Sedeno (1997) followed earlier authors in assuming the distributions of C 2 H 2 and C 2 H 6 to be uniform with latitude and altitude.…”

“…The results from West et al (1992) were used by Friedson et al (1999) to show that the meridional mixing rate of aerosols created in the SL9 collisions was consistent with horizontal eddy mixing derived from the divergence of the Eliasen-Palm flux. Moreno and Sedano (1997) performed dynamical calculations similar to those of West et al (1992) but utilized an aerosol distribution based on analysis of multi-wavelength HST images of Jupiter. These data provide higher spatial resolution than possible with the IUE and Voyager data and the aerosol distribution derived by Moreno and Sedano (1997) has fewer aerosols and therefore less heating than that of West et al (1992) at high northern latitudes.…”

“…Moreno and Sedano (1997) performed dynamical calculations similar to those of West et al (1992) but utilized an aerosol distribution based on analysis of multi-wavelength HST images of Jupiter. These data provide higher spatial resolution than possible with the IUE and Voyager data and the aerosol distribution derived by Moreno and Sedano (1997) has fewer aerosols and therefore less heating than that of West et al (1992) at high northern latitudes. The treatment of gaseous opacities was similar in Moreno and Sedano (1997) and West et al (1992), with the exception that the former authors included radiative cooling by NH 3 , which was neglected in earlier studies.…”

“…The only coefficient available for the 1.1 and 1.3 µm bands are those of Irwin et al (1996), and we use these in our calculations. The choices made here are essentially the same as those of Moreno and Sedano (1997).…”