By A. Coradini, C. Federico, G. Magni (auth.), Angioletta Coradini, Marcello Fulchignoni (eds.)
The quantity gathers the fashionable works by means of members within the NATO complicated research Institute, liThe Comparative examine of the Planets", which was once held at Vulcano (Aeolian Islands) from September 14 to September 25, 1981. The e-book is meant to be a landmark for all these inter ested within the difficulties disclosed during the close-up exploration of planets and satellites, both for pro purposes or just for clinical wisdom. the themes handled crisis all methodologies through which the participants of the sunlight approach were studied and the viewers to whom the amount is addressed is, as well as the specialists, mailllly graduate and post-graduate scholars attending classes in Earth Sciences, Physics and Astro nomy. the purpose we intend to accomplish in modifying this quantity is to provide to planetologists an outline of the current kingdom of information, utilizing the comparative examine of the planets as a foundation on which to construct the topics handled. we predict it truly is one of many fe, ... guides of this sort, including the entire matters about the research of a planet. we are hoping we've succeeded in conveying in the course of the publication the message which was once essentially expressed by means of the academics of the ASI in Vulcano: what counts such a lot at this level of planetary learn is so that it will unmarried out the thrill damental difficulties and select the proper set of knowledge to exploit in forthcoming those problems.
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Additional resources for The Comparative Study of the Planets: Proceedings of the NATO Advanced Study Institute held at Vulcano (Aeolian Islands), Italy, September 14–25, 1981
Example text
The luminosity and surface temperature decrease on a time scale of 5 x 109 years. In fitting the numerical models to the observations it is assumed that the early accretion phases contribute only a small fraction of the total evolutionary time to the present state. l. (6) have presented evolutionary sequences for Jupiter and Saturn with the inclusion of a slow rotation and Hith cores of various masses. The cores consist of Si~, MgO, Fe, and Ni in solar abundance ratios; the envelopes are a homogeneous gas of solar composition.
Space Sci. 153-l58. W. 377406. 1972,NASA TTF-677. 440-443. ,Magni,G. 47-6l. 142-l50,CNRS,Paris. Press. D. ,Reading,Mass. 407-450. J. lOl9-l022. l5)Goldreich,P. J. 1051-1061. 172-l89. ,Federico,C. :l98l,Astron. 173-l85. ,Morfil1,G. 221-227. ,Morfil1,G. 3l6-325. of Arizona Press,Tucson. M. L. of Arizona Press,Tucson. of Arizona Press,Tucson. ,Fulchignoni,M. 65,pp. 21-35. ,Fulchignoni,M. 369-384. :1977,Astrophys. 79-87. Theor. l756-l77l. 517-528. lnt. 302-3l2. A. CORADINI ET AL. 342353. 16-30. 55-60.
1. INTRODUCTION One of the critical periOds of the formation of the solar system occurs when the giant planets condense out of the solar nebula. The processes that occur strongly influence the further evolution of the nebula itself; also the properties of the nebula strongly influence the evolution of the protoplanets. This paper is concerned with two major hypotheses that have been proposed for the early history of the giant planets. An important question that may be asked is whether it is possible to distinguish between these two hypotheses on the basis of our current knowledge of the solar system.