There may be a permanent north–south asymmetry in the zonal wind profile of Uranus. According to high signal-to-noise near-IR observations with the Keck telescope NIRC2 camera, through 2014 the winds north of 60∘N had a constant (zero shear) longitudinal drift rate of 4.1∘/h westward (Sromovsky et al., 2015). Yet the south polar winds in 1986 had strong latitudinal shear, reaching speeds of 8.5∘/h (Karkoschka, 2015). If that asymmetry were a result of extreme seasonal forcing, it might be expected to reverse before the 2030 solstice. However, continued high signal-to-noise near-IR observations from 2015 through 2022 provide little evidence that the north polar winds have changed at all, although there have been changes in the distribution of cloud features used to track those winds and an increase in the brightness of the background haze that makes it harder to detect these small low-contrast features. Between 2015 and 2017, a gap in easily trackable features developed in the 55∘N–60∘N latitude region, and at the northern edge of that gap there was a hint that a dramatic change to the inverted profile might be starting. To further investigate that possible change and to fill in the gap, we developed a new wind measurement technique that was more sensitive to low-contrast spatial structure. Our new method does not confirm any significant wind speed change in the gap, nor at its northern edge.The lifetimes of many of the small discrete polar features are surprisingly long. Many were tracked over time spans over 24 h, and some lasted for weeks. More prominent features seen at low latitudes seem to persist for multiple years and vary in latitude and drift rate in a cyclical fashion. While measurements so far favor a permanent asymmetry in the zonal wind profile of Uranus, the possibility remains that a dramatic circulation change might take place between 2022 and the next solstice in 2030. Using simplified radiation transfer modeling we infer a largely unchanging upper layer of small particles of very low optical depth vertically distributed above an active deeper mid-level layer, at an effective pressure of ∼2–2.5 bar. That middle layer increased in reflectivity at 1.6 μm by more than a factor of 2 from 2015 to 2022 and is the main source of the top-of-atmosphere brightness increase seen over that period, rather than any significant temporal change in polar methane abundance.
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