<P> The tracking of numerous cloud features allowed determination of zonal winds blowing in the upper troposphere of Uranus . At the equator winds are retrograde, which means that they blow in the reverse direction to the planetary rotation . Their speeds are from − 360 to − 180 km / h (− 220 to − 110 mph). Wind speeds increase with the distance from the equator, reaching zero values near ± 20 ° latitude, where the troposphere's temperature minimum is located . Closer to the poles, the winds shift to a prograde direction, flowing with Uranus's rotation . Wind speeds continue to increase reaching maxima at ± 60 ° latitude before falling to zero at the poles . Wind speeds at − 40 ° latitude range from 540 to 720 km / h (340 to 450 mph). Because the collar obscures all clouds below that parallel, speeds between it and the southern pole are impossible to measure . In contrast, in the northern hemisphere maximum speeds as high as 860 km / h (540 mph) are observed near + 50 ° latitude . </P> <P> For a short period from March to May 2004, large clouds appeared in the Uranian atmosphere, giving it a Neptune - like appearance . Observations included record - breaking wind speeds of 820 km / h (510 mph) and a persistent thunderstorm referred to as "Fourth of July fireworks". On 23 August 2006, researchers at the Space Science Institute (Boulder, Colorado) and the University of Wisconsin observed a dark spot on Uranus's surface, giving scientists more insight into Uranus's atmospheric activity . Why this sudden upsurge in activity occurred is not fully known, but it appears that Uranus's extreme axial tilt results in extreme seasonal variations in its weather . Determining the nature of this seasonal variation is difficult because good data on Uranus's atmosphere have existed for less than 84 years, or one full Uranian year . Photometry over the course of half a Uranian year (beginning in the 1950s) has shown regular variation in the brightness in two spectral bands, with maxima occurring at the solstices and minima occurring at the equinoxes . A similar periodic variation, with maxima at the solstices, has been noted in microwave measurements of the deep troposphere begun in the 1960s . Stratospheric temperature measurements beginning in the 1970s also showed maximum values near the 1986 solstice . The majority of this variability is thought to occur owing to changes in the viewing geometry . </P> <P> There are some indications that physical seasonal changes are happening in Uranus . Although Uranus is known to have a bright south polar region, the north pole is fairly dim, which is incompatible with the model of the seasonal change outlined above . During its previous northern solstice in 1944, Uranus displayed elevated levels of brightness, which suggests that the north pole was not always so dim . This information implies that the visible pole brightens some time before the solstice and darkens after the equinox . Detailed analysis of the visible and microwave data revealed that the periodical changes of brightness are not completely symmetrical around the solstices, which also indicates a change in the meridional albedo patterns . In the 1990s, as Uranus moved away from its solstice, Hubble and ground - based telescopes revealed that the south polar cap darkened noticeably (except the southern collar, which remained bright), whereas the northern hemisphere demonstrated increasing activity, such as cloud formations and stronger winds, bolstering expectations that it should brighten soon . This indeed happened in 2007 when it passed an equinox: a faint northern polar collar arose, and the southern collar became nearly invisible, although the zonal wind profile remained slightly asymmetric, with northern winds being somewhat slower than southern . </P> <P> The mechanism of these physical changes is still not clear . Near the summer and winter solstices, Uranus's hemispheres lie alternately either in full glare of the Sun's rays or facing deep space . The brightening of the sunlit hemisphere is thought to result from the local thickening of the methane clouds and haze layers located in the troposphere . The bright collar at − 45 ° latitude is also connected with methane clouds . Other changes in the southern polar region can be explained by changes in the lower cloud layers . The variation of the microwave emission from Uranus is probably caused by changes in the deep tropospheric circulation, because thick polar clouds and haze may inhibit convection . Now that the spring and autumn equinoxes are arriving on Uranus, the dynamics are changing and convection can occur again . </P>

State the length in years of the spring season on uranus
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