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Physics Bulletin, 1982
The study of planets as physical objects goes back to the early 17th century, when Galileo discovered Jupiter's four main satellites and initiated the observations that led to Huyghens' discovery of Saturn's rings. But systematic work in planetary science is a comparatively recent development which has accompanied the rise of modern geophysics and ...
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The study of planets as physical objects goes back to the early 17th century, when Galileo discovered Jupiter's four main satellites and initiated the observations that led to Huyghens' discovery of Saturn's rings. But systematic work in planetary science is a comparatively recent development which has accompanied the rise of modern geophysics and ...
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2001
We have already seen (Sect. 1.2.2) that observation of the basic physical parameters of the planets in the Solar System led naturally to their being divided into two categories: the terrestrial planets (see Chap. 6) and the giant planets. The latter, of which there are four — Jupiter, Saturn, Uranus, and Neptune — are characterized by large diameters ...
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We have already seen (Sect. 1.2.2) that observation of the basic physical parameters of the planets in the Solar System led naturally to their being divided into two categories: the terrestrial planets (see Chap. 6) and the giant planets. The latter, of which there are four — Jupiter, Saturn, Uranus, and Neptune — are characterized by large diameters ...
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2014
The giant planets (Jupiter, Saturn, Uranus, and Neptune), also called the outer planets, are located between 5 and 30 AU from the Sun. They are large bodies, notably exceeding the terrestrial planets in size. Jupiter and Saturn are composed mostly of hydrogen-helium gases, whereas Uranus and Neptune consist of hydrogen-bearing compounds (e.g., methane,
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The giant planets (Jupiter, Saturn, Uranus, and Neptune), also called the outer planets, are located between 5 and 30 AU from the Sun. They are large bodies, notably exceeding the terrestrial planets in size. Jupiter and Saturn are composed mostly of hydrogen-helium gases, whereas Uranus and Neptune consist of hydrogen-bearing compounds (e.g., methane,
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Icarus, 1974
Models of the giant planets were constructed based on the assumption that the hydrogen to helium ratio is solar in these planets. This assumption, together with arguments about the condensation sequence in the primitive solar nebula, yields models with a central core of rock and possibly ice surrounded by an envelope of hydrogen, helium, methane ...
A. G. W. Cameron +2 more
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Models of the giant planets were constructed based on the assumption that the hydrogen to helium ratio is solar in these planets. This assumption, together with arguments about the condensation sequence in the primitive solar nebula, yields models with a central core of rock and possibly ice surrounded by an envelope of hydrogen, helium, methane ...
A. G. W. Cameron +2 more
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Tides on Satellites of Giant Planets
2013The discovery of the satellites of the giant planets started in 1610 when Galileo Galilei pointed his telescope toward Jupiter. Since then observations from Earth- and space-based telescopes and outstanding in-situ observations by several space missions have revealed worlds of great richness and extreme diversity. One major source of energy driving the
Rambaux, Nicolas +1 more
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1973
The result that the giant planets are composed primarily of hydrogen and helium and lighter elements can be placed on a quantitative basis for Jupiter and Saturn because of the accuracy with which relevant equations of state are presently known. Current results are consistent with solar composition for Jupiter and perhaps also for Saturn.
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The result that the giant planets are composed primarily of hydrogen and helium and lighter elements can be placed on a quantitative basis for Jupiter and Saturn because of the accuracy with which relevant equations of state are presently known. Current results are consistent with solar composition for Jupiter and perhaps also for Saturn.
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Aerosols on the Giant Planets and Titan
Space Science Reviews, 2005On the giant planets and Titan, like on the terrestrial planets, aerosols play an important part in the physico-chemistry of the upper atmosphere (P ≤ 0.5 bar). Above all, aerosols significantly affect radiative transfer processes, mainly through light scattering, thus influencing the atmospheric energy budget and dynamics.
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Annual Review of Astronomy and Astrophysics, 2002
▪ Abstract Giant planet research has moved from the study of a handful of solar system objects to that of a class of bodies with dozens of known members. Since the original 1995 discovery of the first extrasolar giant planets (EGPs), the total number of known examples has increased to ∼80 (circa November 2001).
Adam Burrows +2 more
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▪ Abstract Giant planet research has moved from the study of a handful of solar system objects to that of a class of bodies with dozens of known members. Since the original 1995 discovery of the first extrasolar giant planets (EGPs), the total number of known examples has increased to ∼80 (circa November 2001).
Adam Burrows +2 more
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1998
Interior models show that Jupiter and Saturn consist mostly of free hydrogen and helium, while Uranus and Neptune consist mostly of material with a zero-pressure density near 1 g cm−3. The dominant material in Uranus and Neptune is almost certainly ice, while models imply that Jupiter and Saturn each contain roughly one Uranus or Neptune mass of non ...
William B. Hubbard, Morris Podolak
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Interior models show that Jupiter and Saturn consist mostly of free hydrogen and helium, while Uranus and Neptune consist mostly of material with a zero-pressure density near 1 g cm−3. The dominant material in Uranus and Neptune is almost certainly ice, while models imply that Jupiter and Saturn each contain roughly one Uranus or Neptune mass of non ...
William B. Hubbard, Morris Podolak
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Formation of the giant planets
Planetary and Space Science, 1982Observational constraints on interior models of the giant planets indicate that these planets were all much hotter when they formed and they all have rock and/or ice cores of ten to thirty earth masses. These cores are probably soluble in the envelopes above, especially in Jupiter and Saturn, and are therefore likely to be primordial.
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