Journal ArticleDOI
Inversion of Gravity Data for Giant Planets
TLDR
In this article, the authors derived approximate inversion formulas which permit the calculation of the density on an interior level surface of a rotating planet from observed values of J 2, J 4, and J 6, given that the planet is in hydrostatic equilibrium and the density near the surface varies smoothly with depth.About:
This article is published in Icarus.The article was published on 1974-02-01. It has received 20 citations till now. The article focuses on the topics: Neptune & Uranus.read more
Citations
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Optimized Jupiter, Saturn, and Uranus interior models
TL;DR: A method for inverting gravitational data is the basis for the present models of Saturn, Jupiter, and Uranus, which have been computed to the third-order in rotational disturbance to the total potential and yield exact matches for recent, highlyaccurate determinations of gravitational harmonics for these planets.
Journal ArticleDOI
Characterization of exoplanets from their formation III: The statistics of planetary luminosities
TL;DR: In this article, an extensive study of the statistics of planetary luminosities during both formation and evolution is presented, which can be compared with individual directly imaged extrasolar (proto)planets and with statistical results from surveys.
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Further investigations of random models of Uranus and Neptune
TL;DR: In this paper, the authors present a series of computer models for Uranus and Neptune where the interior density distribution is randomly chosen and the only constraints placed on the distribution are that the density does not decrease with decreasing radius, and that the distribution fits the observed mass and gravitational moments of these planets.
Journal ArticleDOI
The structure of the planets Jupiter and Saturn
TL;DR: In this paper, the authors used a fourth-order theory and an equation of state for the molecular hydrogen and helium planetary envelopes taken from the Monte Carlo calculations of Slattery and Hubbard (1976).
The Structure of the Planets Jupiter and Saturn.
TL;DR: In this paper, the authors used a fourth-order theory and an equation of state for the molecular hydrogen and helium planetary envelopes taken from the Monte Carlo calculations of Slattery and Hubbard (1976).
References
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Rapidly rotating stars. i. the self-consistent-field method.
Journal ArticleDOI
Thermal radio emission from Jupiter and Saturn
S. Gulkis,R. Poynter +1 more
TL;DR: In this article, a number of model atmospheres for Jupiter and Saturn were considered and the ammonia abundance below the NH3 cloud level was determined by comparing the observed thermal spectrum of Jupiter and the total spectrum of Saturn with the model calculations.