Results 281 to 290 of about 33,171 (317)
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Scientific American, 1987
The topographies of the major moons of Uranus are described, and reasons for the appearances of the surfaces are given. Oberon and Titania, the two outermost major moons, have similar bulk properties but different appearances. Oberon appears to have been a largely passive structure for incoming projectiles, while Titania's surface shows extensive ...
Robert H. Brown +2 more
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The topographies of the major moons of Uranus are described, and reasons for the appearances of the surfaces are given. Oberon and Titania, the two outermost major moons, have similar bulk properties but different appearances. Oberon appears to have been a largely passive structure for incoming projectiles, while Titania's surface shows extensive ...
Robert H. Brown +2 more
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, 2013 Uranus and Neptune are both thought to have lightning and active chemistry triggered by cosmic ray ionisation. Neptune is expected to have direct condensation of supersaturated vapour onto ions, just like a “Wilson” cloud chamber. There is some evidence that Neptune’s albedo is linked to the flux of galactic cosmic rays entering its atmosphere.
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Journal of Geophysical Research: Space Physics, 1987
Voyager 2 observations have shown that Uranus possesses a well‐developed bipolar magnetotail similar in certain characteristics to that of Earth, in spite of an anomalously large tilt of the planetary magnetic dipole to the rotation axis at Uranus. The intensity of the magnetic field in the tail lobes decreases with increasing distance down the tail ...
Ralph L. McNutt +6 more
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Voyager 2 observations have shown that Uranus possesses a well‐developed bipolar magnetotail similar in certain characteristics to that of Earth, in spite of an anomalously large tilt of the planetary magnetic dipole to the rotation axis at Uranus. The intensity of the magnetic field in the tail lobes decreases with increasing distance down the tail ...
Ralph L. McNutt +6 more
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Science, 1986
The magnetic field experiment on the Voyager 2 spacecraft revealed a strong planetary magnetic field of Uranus and an associated magnetosphere and fully developed bipolar magnetic tail. The detached bow shock wave in the solar wind supersonic flow was observed upstream at 23.7 Uranus radii (1 R U = 25 ...
Ronald P. Lepping +6 more
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The magnetic field experiment on the Voyager 2 spacecraft revealed a strong planetary magnetic field of Uranus and an associated magnetosphere and fully developed bipolar magnetic tail. The detached bow shock wave in the solar wind supersonic flow was observed upstream at 23.7 Uranus radii (1 R U = 25 ...
Ronald P. Lepping +6 more
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Icarus, 1975
Current knowledge of the atmosphere of Uranus is reviewed and specific objectives are suggested for satellite missions to Uranus. The anomalous composition of Uranus makes determinations of its atmospheric composition particularly valuable for testing theories of solar system evolution. The weakness of its atmospheric heating makes the determination of
Peter Stone, Peter Stone
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Current knowledge of the atmosphere of Uranus is reviewed and specific objectives are suggested for satellite missions to Uranus. The anomalous composition of Uranus makes determinations of its atmospheric composition particularly valuable for testing theories of solar system evolution. The weakness of its atmospheric heating makes the determination of
Peter Stone, Peter Stone
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Scientific American, 1987
The rings of Uranus are not all circular; nor do they all lie in the plane of Uranus' equator. The epsilon ring of Uranus, which is the largest and outermost one, ranges in width from 20 to 96 km in proportion to the distance of the ring material from Uranus. Typical rings can be modeled by assuming that its edges are defined by a combination of smooth
Jeffrey N. Cuzzi, Larry W. Esposito
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The rings of Uranus are not all circular; nor do they all lie in the plane of Uranus' equator. The epsilon ring of Uranus, which is the largest and outermost one, ranges in width from 20 to 96 km in proportion to the distance of the ring material from Uranus. Typical rings can be modeled by assuming that its edges are defined by a combination of smooth
Jeffrey N. Cuzzi, Larry W. Esposito
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Icarus, 1979
Several models for the atmosphere of Uranus are considered. If the H2 abundance is less than 250 km-am and the internal heat source is only a few percent of the total emitted energy then the cloud at the base of the atmosphere may be composed of solid CH4 particles, while if the H2 abundance is greater than 250 km-am or if the internal heat source is ...
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Several models for the atmosphere of Uranus are considered. If the H2 abundance is less than 250 km-am and the internal heat source is only a few percent of the total emitted energy then the cloud at the base of the atmosphere may be composed of solid CH4 particles, while if the H2 abundance is greater than 250 km-am or if the internal heat source is ...
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Science, 1977
An upper limit of 0.05 is established for the geometric albedo of the newly discovered rings of Uranus. In view of this very low albedo, the particles of the rings cannot be ice-covered as are those of rings A and B of Saturn.
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An upper limit of 0.05 is established for the geometric albedo of the newly discovered rings of Uranus. In view of this very low albedo, the particles of the rings cannot be ice-covered as are those of rings A and B of Saturn.
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1994
Travelling in excess of 20 km s−1 in early 1986, the Voyager 2 spacecraft streaked past Uranus on its continuing journey through the outer Solar System. In its brief encounter, Voyager 2 returned more information on Uranus, its rings and its satellites than had been accumulated in the 205 years since the discovery of this, the seventh planet from the ...
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Travelling in excess of 20 km s−1 in early 1986, the Voyager 2 spacecraft streaked past Uranus on its continuing journey through the outer Solar System. In its brief encounter, Voyager 2 returned more information on Uranus, its rings and its satellites than had been accumulated in the 205 years since the discovery of this, the seventh planet from the ...
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Scientific American, 1987
The giant blue-green planet visited last January by Voyager 2 has one pole pointing toward the sun, and its magnetic field is askew. Its atmosphere is dense and icy, yet its winds resemble the earth's. ; © 1987 Scientific American, a division of Nature America, Inc.
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The giant blue-green planet visited last January by Voyager 2 has one pole pointing toward the sun, and its magnetic field is askew. Its atmosphere is dense and icy, yet its winds resemble the earth's. ; © 1987 Scientific American, a division of Nature America, Inc.
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