Phase dispersion relation of the 5‐micron hot spot wave from a long‐term study of Jupiter in the visible

Abstract

[1] We present a long-term study at visible wavelengths of the motions and spatial distribution of the hot spots at 7°N of Jupiter. This research involves seven years of observations of the planet between 1979 and 2002 and includes data from Voyagers 1 and 2, Hubble Space Telescope, and a number of ground-based observatories. Our analysis of the North Equatorial Belt (NEB) dark projections (DPs) velocities and wave numbers showsthatadispersionrelationship exists,withtheDPsvelocity(rangingfrom97to113ms À1 ) slightly increasing with wave number (ranging from 6 to 20, although usually 8-12). We interpret this relationship in terms of a superposition of equatorial Rossby waves traveling along the planet and confined to the upper troposphere. The resulting equivalent depth for the waves on an incompressible fluid is 1-2 km, and they move relative to a background flow with speed 140 m s À1 , a result in good agreement with previous analysis of the wave interpretation for hot spot motions as observed in the infrared.Citation: Arregi, J., J. F. Rojas, A. Sánchez-Lavega, and A. Morgado (2006), Phase dispersion relation of the 5-micron hot spot wave from a long-term study of Jupiter in the visible,

Dynamics and Clouds in Jupiter Equatorial Zone

“…From our measurements of the movement of the different dark projection groups we obtained the dispersion relationship shown in Fig. 3 [3]. Interestingly these values are similar to the ones that Ortiz et al [4] found when studying the hot spots movement in the IR.…”

Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival

“…The main article covers two newly-identified wave patterns in the 0-30 • N domain, but the data presented throughout the article also shows thermal contrasts associated with a third wave on the prograde NEBs jet between 6-9 • N. This pattern of visibly-dark, longitudinallyelongated 'hotspots' and adjacent bright fans of material (referred to as plumes, although these are not always associated with convection) that can be seen near 8 • N in reflected sunlight [Allison, 1990;Baines et al, 2002;Arregi et al, 2006;Choi et al, 2013], infrared [Or- Fletcher et al, 2016], and radio-wave observations [de Pater et al, 2016;Cosentino et al, 2017]. This chain moves slowly westward with respect to the rapid eastward flow of the NEBs, and has been interpreted as an equatorial Rossby wave pattern [Showman and Ingersoll, 1998;Showman and Dowling, 2000;Friedson, 2005], with rising air and condensation in the plumes and descent and aerosol-clearing in the hotspots.…”

“…Note that this section does not deal with the trapped equatorial Rossby wave pattern on the NEBs [and its associated hotspots and plumes, Allison, 1990;Ortiz et al, 1998;Showman and Dowling, 2000;Baines et al, 2002;Friedson, 2005;Arregi et al, 2006;Choi et al, 2013].…”

Jupiter’s zonal winds and their variability studied with small-size telescopes

“…(1) the South Temperate Belt was faded, except for a turbulent sector extending about 80 • in longitude, with a detached oval BA characterized by its ringed structure and the accompanying small, dark cyclone and short turbulent area; (2) there was a well-developed gray belt in the STrZ contiguous to the SEB, making this belt appear wider in latitude than it usually is; (3) the SEB was fully recovered as a low albedo band from its last fade (Pérez-Hoyos et al 2012); (4) no large and conspicuous "dark projections" were present at the equatorward edge of the NEB (these are the low-albedo visible counterparts to the 5-μm hot spots; Arregi et al 2006). We show that this is an important aspect affecting the wind profile; (5) on the NEB poleward side, three large barges dominate the scene (about five in total were present); (6) the north tropical zone (NTrZ) was a prominent zone, but the NTB was faint with small-scale features.…”