It is much slower than is typical for Jovian planets.
It is much faster than is typical for Jovian planets.
The equator rotates much faster than the poles.
The axis is nearly parallel to the plane of its orbit.
Are not massive enough.
Rotate too slowly.
Have magnetic fields that are much too weak.
Are not rich enough in hydrogen.
There is no liquid metallic core.
Clouds form very deep in the atmosphere.
No clouds form in the pure hydrogen atmosphere.
There is no differential rotation.
Highly inclined to the axis of rotation.
Produced by disturbances caused by the orbits of the moons.
Linked to the solar wind.
During an eclipse of one of the moons by the rings.
By Voyager 1.
During an occultation of a star.
During an eclipse of Uranus by the rings.
Being ejected from volcanoes on the surfaces of geologically active satellites of the planets.
Radiation from the magnetospheres of the planets interacting with chemicals in the ring particles.
Forming in a region so far from the sun that only icy particles can exist.
Collisions with small icy particles from the outer reaches of the solar system.
Both of them have very small masses for Jovian planets.
Their surfaces are covered with water and their clouds are very thin.
Their atmospheres absorb blue light very efficiently.
Their atmospheres absorb red light very efficiently.