Abstract
Mid-infrared 7–20 μm imaging of Jupiter from ESO’s Very Large Telescope (VLT/VISIR) demonstrate that the increased albedo of Jupiter’s South Equatorial Belt (SEB) during the ‘fade’ (whitening) event of 2009–2010 was correlated with changes to atmospheric temperature and aerosol opacity. The opacity of the tropospheric condensation cloud deck at pressures less than 800 mbar increased by 80% between May 2008 and July 2010, making the SEB (7–17°S) as opaque in the thermal infrared as the adjacent equatorial zone. After the cessation of discrete convective activity within the SEB in May 2009, a cool band of high aerosol opacity (the SEB zone at 11–15°S) was observed separating the cloud-free northern and southern SEB components. The cooling of the SEBZ (with peak-to-peak contrasts of 1.0 ± 0.5 K), as well as the increased aerosol opacity at 4.8 and 8.6 μm, preceded the visible whitening of the belt by several months. A chain of five warm, cloud-free ‘brown barges’ (subsiding airmasses) were observed regularly in the SEB between June 2009 and June 2010, by which time they too had been obscured by the enhanced aerosol opacity of the SEB, although the underlying warm circulation was still present in July 2010. Upper tropospheric temperatures (150–300 mbar) remained largely unchanged during the fade, but the cool SEBZ formation was detected at deeper levels ( p > 300 mbar) within the convectively-unstable region of the troposphere. The SEBZ formation caused the meridional temperature gradient of the SEB to decrease between 2008 and 2010, reducing the vertical thermal windshear on the zonal jets bounding the SEB. The southern SEB had fully faded by July 2010 and was characterised by short-wave undulations at 19–20°S. The northern SEB persisted as a narrow grey lane of cloud-free conditions throughout the fade process. The cool temperatures and enhanced aerosol opacity of the SEBZ after July 2009 are consistent with an upward flux of volatiles (e.g., ammonia-laden air) and enhanced condensation, obscuring the blue-absorbing chromophore and whitening the SEB by April 2010. These changes occurred within cloud decks in the convective troposphere, and not in the radiatively-controlled upper troposphere. NH 3 ice coatings on aerosols at p < 800 mbar are plausible sources of the suppressed 4.8 and 8.6-μm emission, although differences in the spatial distribution of opacity at these two wavelengths suggest that enhanced attenuation by a deeper cloud ( p > 800 mbar) also occurred during the fade. Revival of the dark SEB coloration in the coming months will ultimately require sublimation of these ices by subsidence and warming of volatile-depleted air.
Highlights
Jupiter’s axisymmetric structure, consisting of bright zones and dark brown 3 belts, can undergo dramatic visible changes over short time scales
This following sections compare temperature and aerosol distributions derived from Very Large Telescope (VLT) 7-20 μm filtered imaging to both Infrared Telescope Facility (IRTF) 4.8-μm images of deep cloud opacity and amateur imaging of the visible coloration to reveal the sequence of changes occurring during the South Equatorial Belt (SEB) fade
Initial State of the SEB (Pre-May 2009) Filamentary turbulent convective activity usually dominates the SEB to the northwest of the Great Red Spot (GRS) in a region known as the ‘GRS wake.’
Summary
Jupiter’s axisymmetric structure, consisting of bright zones and dark brown 3 belts, can undergo dramatic visible changes over short time scales. The SEB is a site of intense convective activity and lightning storms (Ingersoll et al, 2004), and is one of the few locations where spectroscopically identifiable ammonia clouds (SIACs, Baines et al, 2002) have been observed This activity and the dark colouration of the SEB were completely absent when Jupiter emerged from behind the Sun during the 2010 apparition, replaced by the pale ‘faded’ state (Fig. 2c). This missing jovian belt captured the imagination of amateur and professional astronomers alike, and it prompted a program of thermal infrared imaging of Jupiter’s faded SEB from the ESO Very Large Telescope (VLT) at Cerro Paranal in Chile. Af45 ter the cessation of turbulent rifting and convective events to the northwest of the 46 GRS, the SEB (7-17◦S planetocentric latitude) fades to a pale colour over a mat ter of months, obscuring the southern component of the SEB (SEBs, 15-17◦S)
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