Physical processes in the protoplanetary disk

Details Physical processes in the protoplanetary disk Physical processes in the protoplanetary disk

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ssrv...56...65v&link_type=abstract

(Analysis of samples from solar system bodies with emphasis on existing and emerging technologies; Proceedings of the Internatio

Computer Science

Emerging Technologies

3

Accretion Disks, Cosmic Dust, Gravitational Collapse, Planetary Evolution, Protoplanets, T Tauri Stars, Chondrule, Interstellar Matter, Stellar Envelopes, Turbulence Effects, Planets, Protoplanets, Evolution, Turbulence, Chemistry, Fractionation, Grain Size, Electrical Effects, Heating, Mineralogy, Morphology, Dust, Alteration, Sedimentation, Planetesimals, Formation, Theoretical Studies, Models, Origin, Gravity Effects, Cosmochemistry, Acceleration, Temperature, Solar System

Scientific paper

Protoplanetary evolution is discussed in both its global and local aspects. The global turbulent evolution implies large scale average chemical fractionation and chondrule-sized grains as the building blocks of planetary and possibly also cometary material. Local processes such as electric discharges and associated flash heating of grains allow for chemical, mineralogical, and morphological alterations of the disk material. Large scale turbulence keeps the disk well stirred; however, time dependent (or intermittent) turbulence (e.g., associated with optical depth variations) could lead to dust sedimentation within the disk and subsequent planetesimal formation. Recent relevant astronomical observations of young T Tauri stars are briefly reviewed.

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