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Atmospheric structure and dynamics as the cause of ultraviolet markings in the clouds of Venus


When seen in ultraviolet light, Venus has contrast features that arise from the non-uniform distribution of unknown absorbers within the sulphuric acid clouds1,2,3 and seem to trace dynamical activity in the middle atmosphere4. It has long been unclear whether the global pattern arises from differences in cloud top altitude (which was earlier3 estimated to be 66–72 km), compositional variations or temperature contrasts. Here we report multi-wavelength imaging that reveals that the dark low latitudes are dominated by convective mixing which brings the ultraviolet absorbers up from depth. The bright and uniform mid-latitude clouds reside in the ‘cold collar’, an annulus of cold air characterized by 30 K lower temperatures with a positive lapse rate, which suppresses vertical mixing and cuts off the supply of ultraviolet absorbers from below. In low and middle latitudes, the visible cloud top is located at a remarkably constant altitude of 72 ± 1 km in both the ultraviolet dark and bright regions, indicating that the brightness variations result from compositional differences caused by the colder environment rather than by elevation changes. The cloud top descends to 64 km in the eye of the hemispheric vortex, which appears as a depression in the upper cloud deck. The ultraviolet dark circular streaks enclose the vortex eye and are dynamically connected to it.

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Figure 1: False-colour image of Venus taken by VMC from a distance of 30,000 km in the ultraviolet filter.
Figure 2: Thermal infrared spectroscopy of the Venus southern hemisphere by VIRTIS.
Figure 3: Altimetry of the cloud tops.
Figure 4: Composite false colour views of the southern hemisphere.
Figure 5: Sketch of the global morphology of the cloud top.


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We thank the European Space Agency (ESA) for its efforts and dedication in implementation of the Venus Express mission and the teams at ESOC and ESAC for operational support. We thank the UK Science and Technology Facilities Council, Italian (ASI) and French (CNES) space agencies for support. N.I.I. acknowledges support from the Russian Foundation for Basic Research.

Author Contributions D.V.T. led the work and studied correlations of the ultraviolet and thermal infrared features in VMC and VIRTIS images; F.W.T. worked on meteorological aspects; H.S. is the Venus Express Project Scientist; N.I.I. derived the maps of cloud top altitude from the VIRTIS spectra; W.J.M., G.P. and P.D. are the Principal Investigators of VMC and VIRTIS experiments and led the observations. All authors discussed the results and commented on the manuscript.

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Correspondence to Dmitry V. Titov.

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Titov, D., Taylor, F., Svedhem, H. et al. Atmospheric structure and dynamics as the cause of ultraviolet markings in the clouds of Venus. Nature 456, 620–623 (2008).

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