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Although there is no well-defined solid surface within Uranus's interior, the outermost part of Uranus's gaseous envelope that is accessible to remote sensing is called its atmosphere. [18] Remote-sensing capability extends down to roughly 300 km below the 1 bar (100 kPa) level, with a corresponding pressure around 100 bar (10 MPa) and ...
Temperature profile of the Uranian troposphere and lower stratosphere. Cloud and haze layers are also indicated. The Uranian atmosphere can be divided into three main layers: the troposphere, between altitudes of −300 [a] and 50 km and pressures from 100 to 0.1 bar; the stratosphere, spanning altitudes between 50 and 4000 km and pressures between 0.1 and 10 −10 bar; and the thermosphere ...
In the 1990s, it was determined that Uranus and Neptune were a distinct class of giant planet, separate from the other giant planets, Jupiter and Saturn, which are gas giants predominantly composed of hydrogen and helium. [1] Neptune and Uranus are now referred to as ice giants. Lacking well-defined solid surfaces, they are primarily composed ...
Uranus is an unusual world that spins on its side with a 98-degree tilt, which means the icy planet experiences seasons in an extreme way. One year on Uranus lasts around 84 Earth years, and for ...
Alone but certainly unique, Uranus rotates at a nearly 90-degree angle and is surrounded by 13 icy rings. Images of which were captured in rich detail last year by the James Webb Space Telescope .
In particular, the spacecraft’s observations of Uranus’ protective magnetosphere were wildly different from astronomers’ expectations. ... (4,000 meters) below the ocean’s surface. ...
Uranus is an oblate spheroid, which causes its visible area to become larger when viewed from the poles. This explains in part its brighter appearance at solstices. [16] Uranus is also known to exhibit strong zonal variations in albedo (see above). [10] For instance, the south polar region of Uranus is much brighter than the equatorial bands. [3]
The major moons of Uranus are thought to have formed in the accretion disc, which existed around Uranus for some time after its formation or resulted from a large impact suffered by Uranus early in its history. [31] [32] This view is supported by their large thermal inertia, a surface property they share with dwarf planets like Pluto and Haumea ...