Jovian Planetary Waves  J. Harrington (NRC/NASA GSFC), D. Deming
(NASA GSFC)  We have found over two dozen discrete, linearly-
propagating, periodic features in 5-m m images of Jovian cloud
opacities (J. Harrington et al. 1996, Icarus 124, 32-44).
Numerous spatially-sinusoidal temperature oscillations also
appear in several passbands between 7 and 19 (D. Deming et al.
1997, Icarus 126, 301-312). Both types of Jovian planetary-scale
features are zonally-oriented. They have always been detected
when sought (1989, '91, '92, '93), and some individual features
persist 100 Earth days or longer. These features are
superficially consistent with Rossby waves, but they do not
follow a simplistic dispersion relation based on cloud-top wind
speeds. Planetary wavenumbers are never larger than 15,
consistent with predictions based on the Rhines scale for
Jupiter.  There are many outstanding phenomenological questions:
Where and how are the waves driven? How are waves at different
atmospheric levels related? What are their t