Keck adaptive optics images of Jupiter’s north polar cap and Northern Red Oval

We present observations at near-infrared wavelengths (1–5 μm) of Jupiter’s north polar region and Northern Red Oval (NN-LRS-1). The observations were taken with the near-infrared camera NIRC2 coupled to the adaptive optics system on the 10-m W.M. Keck Telescope on UT 21 August 2010. At 5-μm Jupiter’s disk reveals considerable structure, including small bright rings which appear to surround all small vortices. It is striking, though, that no such ring is seen around the Northern Red Oval. In de Pater et al. [2010a. Icarus 210, 742–762], we showed that such rings also exist around all small vortices in Jupiter’s southern hemisphere, and are absent around the Great Red Spot and Red Oval BA. We show here that the vertical structure and extent of the Northern Red Oval is very similar to that of Jupiter’s Red Oval BA. These new observations of the Northern Red Oval, therefore, support the idea of a dichotomy between small and large anticyclones, in which ovals larger than about two Rossby deformation radii do not have 5-μm bright rings. In de Pater et al. [2010a. Icarus 210, 742–762], we explained this difference in terms of the secondary circulations within the vortices. We further compare the brightness distribution of our new 5-μm images with previously published radio observations of Jupiter, highlighting the depletion of NH3 gas over areas that are bright at 5 μm.

► At 5 μm, Jupiter’s disk reveals a lot of structure, including small bright rings around all small vortices.
► No 5-μm bright rings are seen around the GRS, Oval BA, or the Northern Red Oval.
► The size, color and vertical structure of the Northern Red Oval is similar to that of Red Oval BA.
► This difference can be explained in terms of the secondary circulations within the vortices.
► A comparison of the brightness distribution of 5-μm images with previously published radio observations of Jupiter, highlights the depletion of NH3 gas over areas that are bright at 5 μm.