The 2007 Jupiter's North Temperate Belt Disturbance: III. Dynamical models.

Details The 2007 Jupiter's North Temperate Belt Disturbance: III. Dynamical models. The 2007 Jupiter's North Temperate Belt Disturbance: III. Dynamical models.

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.1902h&link_type=abstract

American Astronomical Society, DPS meeting #39, #19.02; Bulletin of the American Astronomical Society, Vol. 39, p.444

Astronomy and Astrophysics

Astronomy

Scientific paper

The eruption of the 2007 North Temperate Belt (NTB) Disturbance was triggered by the development of two bright spots located at the peak of the 23.5° North jet. We propose these spots were of convective origin because: i) They reached levels well above the tropopause, ii) They developed quickly (in less than 10 hr) and, iii) They produced fresh and bright clouds torn apart by the jet shear leeward of the plumes. We studied the conditions required to form these storms using a three-dimensional model of moist convection. In order for the storms to reach these vertical levels they must have their root on the water cloud base at 6 bar depth, the water abundance should be at least 2-3 times solar and the tropopause should be 2-5 K cooler than the Voyager IRIS or Cassini CIRS thermal temperatures close to the tropopause. The interaction of the convective plumes with the jet was simulated using a simple two-dimensional model where mass continuity and a divergent source for the plume are considered. The impact of the plumes within the NTB jet was simulated using the EPIC code where the convective plumes were introduced as a heat source. The outcome of the simulations was very sensitive to the shape of the jet before the onset of the perturbations but the plumes did not change significantly the amplitude of the jet. In order to reproduce the observed patterns of the observed turbulence structures, the jet must extend in depth with constant or slightly increasing winds down to the water condensation level at 6 bar.
Acknowledgements:
This work was supported by the MEC Plan Nacional de Astronomía y Astrofísica, Grupos UPV and Fondos FEDER and made use of computing facilities at CESCA in Barcelona with the help of the Ministerio de Educación y Ciencia.

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