A survey of the outer planets Jupiter, Saturn, Uranus, Neptune, Pluto, and their satellites

Newburn, R. L.; Gulkis, S.

doi:10.1007/bf02432098

Cited by 109 publications

(12 citation statements)

References 283 publications

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“…These rotational effects are nevertheless somewhat weaker than those expected from a gravitating body of uniform density, indicating that the density of Jupiter increases with depth to a central value of about three times the mean density (see Michaux (1967) or Newburn & Gulkis (1973). Allen (1963) or Newburn & Gulkis (1973). Allen (1963), Cook (1973), Michaux (1967), Newburn & Gulkis (1973) and Warwick (1967Warwick ( , 1970.…”

Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 95%

“…The rapid spin of the planet on its axis, with a period of just under 10 h, produces a noticeable oblateness in the appearance of the visible disk in a telescope and the concomitant distortion of the gravitational field of the planet gives rise to measur able perturbations in the orbits of the innermost satellites (see table 3). These rotational effects are nevertheless somewhat weaker than those expected from a gravitating body of uniform density, indicating that the density of Jupiter increases with depth to a central value of about three times the mean density (see Michaux (1967) or Newburn & Gulkis (1973). Allen (1963) or Newburn & Gulkis (1973).…”

Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 96%

“…Allen (1963) or Newburn & Gulkis (1973). Allen (1963), Cook (1973), Michaux (1967), Newburn & Gulkis (1973) and Warwick (1967Warwick ( , 1970.…”

Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 99%

“…It is possible at some wavelengths to see below the upper layer of white ammonia cirrus through a clear region to a more substantial and colourful cloud deck which, according to Lewis (1969;see also Hunt 1973;Taylor & Hunt 1973) consists mainly of particles of ammonium hydrosulphide (NH4SH). Recent work on the nature of Jupiter's striking and variable colours (see figure 1) indicates that they might be largely due to the presence at the NH4SH cloud deck of various products of photolysis of NH3, H 2S and other compounds by solar ultraviolet light (see Lewis & Prinn 1970;Owen & Mason 1969;Owen & Westphal 1972; for further references see Kuiper 1972;Newburn &Savage &Danielson 1968).…”

Section: Jupiter and Satumentioning

confidence: 99%

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Jupiter and Saturn

1974

Proc. R. Soc. Lond. A

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Jupiter, the largest planet, and Saturn, the second largest, contain nine-tenths of the material of the solar system outside the Sun and most of the angular momentum of the solar system is associated with their orbital motion. Both planets rotate very rapidly (rotation periods ~ 10 h) and possess rich satellite systems. Owing to their strong gravitational fields and low surface temperatures, Jupiter and Saturn may, unlike the ‘terrestrial’ planets, be fairly close in chemical composition to the primordial material out of which the solar system originally formed; they consist mainly of hydrogen, much of which is compressed to a metallic form. Jupiter is the only planet other than Earth showing evidence of a general magnetic field. Absorption of incident solar energy accounts for less than one-half the estimated total thermal (infrared) radiation emitted by Jupiter and Saturn. The balance is probably due to internal heat sources and could be accounted for in terms of a gravitational contraction at about 0.1 cm/year. The outward flow of heat should maintain the atmospheric temperature gradients close to their adiabatic values, which is a significant result for theories of atmospheric motions (see appendix A). These theories are largely concerned with explaining the rough alinement of clouds in bands parallel to the equator, the presence of strong eastward equatorial currents, the occurrence of transient spots and other irregular markings and, in the case of Jupiter, the nature of the enigmatic Great Red Spot. Jupiter, unlike Saturn, is a strong emitter of non-thermal radio noise on decametre and decimetre wavelengths. Plausible theories of this radio emission invoke a strong Jovian dipole magnetic field and an associated system of van Allen-type ‘radiation’ belts of electrically-charged particles extending beyond and interacting with the first Galilean satellite Io. The most likely source of the Jovian magnetic field - which theories of Jupiter’s internal constitution must now take properly into account - is a hydromagnetic dynamo (see appendix B) associated with fluid motions in the electrically-conducting parts of Jupiter’s interior. The absence of a non-thermal component in Saturn’s radio spectrum implies that radiation belts cannot form around that planet, possibly because Saturn is non-magnetic or, if it is magnetic, because charged particles in the vicinity of Saturn are rapidly removed through interactions with Saturn’s rings. Modern research on Jupiter and Saturn is based on a rich variety of data, soon to be augmented by observations from space-craft. Future progress with the theoretical interpretation of these data in terms of improved models of the structure and evolution of the giant planets will involve not only the further application of a wide range of established knowledge but also the development of new ideas in several areas of basic science. The paper ends with two appendices, on the dynamics of rapidly rotating non-homogeneous fluids and on hydromagnetic dynamos.

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Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 95%

Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 96%

“…Allen (1963) or Newburn & Gulkis (1973). Allen (1963), Cook (1973), Michaux (1967), Newburn & Gulkis (1973) and Warwick (1967Warwick ( , 1970.…”

Section: J U P I T E R 'S M a In C H A R A C T E R Is T Ic Smentioning

confidence: 99%

Section: Jupiter and Satumentioning

confidence: 99%

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Jupiter and Saturn

1974

Proc. R. Soc. Lond. A

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“…The method will now be applied to six cases of the restricted Jupiter orbiter problem, namely, where the values of at and mass-ratio/h (Jupiter = 1) are those given by Newburn and Gulkis (1973). Then, 0h is determined by ~i < 1.…”

Section: Applications Of Phase Equilibriamentioning

confidence: 98%

Introduction to the restricted Jupiter orbiter problem

Heppenheimer¹

1976

Celestial Mechanics

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Abstract. We consider a restricted six-body problem, consisting of Jupiter, the four Galilean satellites, and an orbiter. The Galilean satellites' orbits are circular and coplanar; Io, Europa, and Ganymede are in exact resonance; their mean longitudes obey the Laplace relation. We seek periodic orbits which avoid close approaches to any satellite; such orbits are of interest for mission planning. They are approximated as equilibrium points of sets of variational equations associated with time-averaged disturbing functions. Stability of the solutions is also determined. The orbits of greatest interest are: Planar: twice Callisto's period, eccentricity ~<0.6 Planar: four times Callisto's period, eccentricity ~0.75 Slightly inclined: twice Callisto's period, eccentricity arbitrary Planar: 4/5 or 5/4 Europa's period.

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Interior Structure of Saturn Inferred from Pioneer 11 Gravity Data

Macfarlane

Hubbard

Anderson

et al. 1980

1980, Pioneer Saturn

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The structure of Saturn is studied via a fourth-order theory for rotating planets and equations of state for the envelope which depend parametrically on the helium abundance, on the starting temperature for the adiabat, and on adopted forms of the pressure-density curve in the region of transition from molecular to metallic hydrogen. Models are congtrained by the values of J2 and J4 obtained from the Pioneer-Saturn celestial mechanics experiment. Equations of state are tested by computing Jupiter models, which can now be subjected to a more stringent comparison with observed zonal harmonics. We find that Saturn has a low-density hydrogen-helium envelope with no evidence for enhancement of H20, CH4, or other abundant compounds. Such compounds are presumably located near the core. The helium mass abundance for Saturn's envelope appears to be in the range of--•0.12 to --•0.19, but this result is very model-dependent. The helium abundance in the envelope of Jupiter is apparently very similar to that of Saturn. thermodynamics of the envelope. In the ideal gas region, adiabats are calculated taking into account quantized vibration and rotation of the H: molecule. As discussed by Hubbard and MacFarlane [1980], for p > 0.005 g/½m 3 it is necessary to continue the adiabatic curves by means of analytic fits to Monte Carlo data for the thermodynamic parameters of compressed H:-He mixtures. Data used for this purpose are given in Tables 1 and 2. These data are an extension of the results given by Hubbard and MacFarlane [1980]. We have computed thermodynamics for pure molecular hydrogen and for a ratio of hydrogen molecules to helium atoms of 16/3 (corresponding to Y = 0.27). At these densities, temperatures are high enough for the classical approximation to the vibration and rotation of H: molecules to be valid. The characteristic vibration and rotation temperatures are assumed to be independent of density. Here ¾ is the value of 0 In T/O In p along an adiabat. Procedures for determining adiabats from such data are discussed by Hubbard and MacFarlane. For an arbitrary value of Y the correct adiabat is obtained from an interpolation between the two tables.

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A survey of the outer planets Jupiter, Saturn, Uranus, Neptune, Pluto, and their satellites

Cited by 109 publications

References 283 publications

Jupiter and Saturn

Jupiter and Saturn

Introduction to the restricted Jupiter orbiter problem

Interior Structure of Saturn Inferred from Pioneer 11 Gravity Data

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