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Structure of the satellitary accretion disk of Saturn |
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| Authors: | A Coradini G Magni |
| Institution: | Istituto di Astrofisica Spaziale, CNR, Frascati, Rome, Italy |
| Abstract: | A detailed computation on the equilibrium structure of an accretion disk around Saturn from which the regular satellites presumably originated is reported. Such a disk is the predecessor of the self-dissipating disk that is formed when the mass infall stops (Cassen and Moosman, 1981, Icarus48, 353–376). When determining the disk structure local energy balance was assumed. Convention was taken into account by introducing local energy dissipation and, in an approximate manner, sonic convection. Changes in the disk structure were investigated by varying the free parameters, i.e., the external flux from both the protosun and the protoplanet, the abundance of dust and the strength of turbulence. It has been verified that the external energy flux does not play an important role in the evolution of the disk structure. Models characterized by either longer times (?3 103 year) or a noticeable depletion of condensable elements (10?2 times less than the solar value) have a total mass of the order of 0.34?0.1 times the mass of the regular satellites increased by the mass of the light elements. Low turbulence models (Reynolds critical number ) are characterized approximately by a total mass twice as large the mass of the regular satellites. All the studied models present a temperature distribution that allows the condensation of iron, silicate, and, in the outer regions, ice grains. All models but the one with 10?2 of the solar value of condensable elements are characterized by a wide convective region that contains the formation zone of the regular satellites. |
| Keywords: | To whom correspondence should be addressed: Reparto di Planetologia Viale dell' Università 11 00185 Rome Italy |
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