Results 121 to 130 of about 24,216 (169)
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Composition and structure of planetary atmospheres
Space Science Reviews, 1971Donald M Hunten
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Dipole structure of planetary atoms
Physical Review Letters, 1992Using resonant multiphoton laser excitation in combination with temporarily applied electric fields we have excited high-lying planetary states in strontium. Thereby, the angular momenta were high enough to prevent penetration of the ${\mathrm{Sr}}^{++}$ core, as well as the mutual penetration of the two excited wave functions. Analysis of the spectra (
, Eichmann, , Lange, , Sandner
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Formation of a filamentary structure in planetary nebulae
Astrophysics and Space Science, 1995Intricate filamentary structure and multiple shell—like appearance are very common phenomena in Planetary Nebulae.
G. Pascoli, J. Leclercq
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An experiment to determine the structure of a planetary atmosphere
5th Annual Meeting and Technical Display, 1968Planetary atmosphere structure and mean molecular weight determination from onboard measurements tested at high altitude in earth atmosphere, based on NASA ...
SIMON C. SOMMER, LAYTON YEE
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On the radial structure of planetary rings
International Astronomical Union Colloquium, 1984ABSTRACTA ring of particles in orbit about a planet experiences a viscous shear stress due to the radial gradient of orbital velocity. This stress tends to spread the ring with time. At low optical depth (τ ≲ 0.5), and again at high optical depth (τ ≳ 2), the shear stress is an increasing function of optical depth.
A.W. Harris, W.R. Ward
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2011
Models of the interior structure of a ▶ planet or ▶ satellite give the variations of thermodynamic state variables as functions of radius (starting at the center) or depth (starting at the surface). The thermodynamic state variables are pressure, temperature, density (or specific volume), and the concentration of chemical species.
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Models of the interior structure of a ▶ planet or ▶ satellite give the variations of thermodynamic state variables as functions of radius (starting at the center) or depth (starting at the surface). The thermodynamic state variables are pressure, temperature, density (or specific volume), and the concentration of chemical species.
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2002
Abstract The material in a given orbit coalesces into a planet for reasons that are not completely clear and, in the case of the Earth, the planet probably underwent a meltdown. The energy for this process came from gravitational potential energy, kinetic energy of the components, heat of radioactive decay and radiant energy from the sun.
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Abstract The material in a given orbit coalesces into a planet for reasons that are not completely clear and, in the case of the Earth, the planet probably underwent a meltdown. The energy for this process came from gravitational potential energy, kinetic energy of the components, heat of radioactive decay and radiant energy from the sun.
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The Structuring of Planetary Nebulae
AIP Conference Proceedings, 2005This paper discusses some features in Planetary Nebulae and Protoplanetary Nebulae that are addressed by several works on MHD. We review different scenarios for the origin of magnetized winds, either for Protoplanetary Nebulae or Planetary Nebulae, and discusses the production of axisymmetric flows, the confinement of flows and the production of jets ...
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STRUCTURE OF PLANETARY ATMOSPHERES
AIAA Journal, 1963The temperature, composition, pressure, and other properties of the atmospheres of Earth, Mars, Venus, and Jupiter are reviewed in the light of the most recent observational results. Several models for the Venus atmosphere are described. (D.L.C.)
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Interpretation and analysis of planetary structures
Journal of Structural Geology, 2010Structural geology is an integral part of planetary science. Planetary structures provide the framework for determining the character and sequence of crustal deformation while simultaneously establishing the observational basis required to test geodynamic hypotheses for the deformation of planetary and satellite lithospheres.
Schultz, Richard A. +4 more
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