Protostellar collapse: rotation and disk formation

Abstract

We present some important conclusions from recent calculations pertaining to the collapse of rotating molecular cloud cores with axial symmetry, corresponding to evolution of young stellar objects through classes 0 and begin of class I. Three main issues have been addressed: (1) The typical timescale for building up a preplanetary disk - once more it turned out that it is of the order of one free-fall time which is decisively shorter than the widely assumed timescale related to the so-called 'inside-out collapse'; (2) Redistribution of angular momentum and the accompanying dissipation of kinetic (rotational) energy - together these processes govern the mechanical and thermal evolution of the protostellar core to a large extent; (3) The origin of calcium-aluminium-rich inclusions (CAIs) - due to the specific pattern of the accretion flow, material that has undergone substantial chemical and mineralogical modifications in the hot (exceeding 900 K) interior of the protostellar core may have a good chance to be advectively transported outward into the cooler remote parts (beyond 4 AU, say) of the growing disk and to survive there until it is incorporated into a meteoritic body.

4 pages, 4 figures

References in corpus (3)

• Theory of Star Formation
• Radiative transfer and the energy equation in SPH simulations of star formation
• Two-Dimensional Transport of Solids in Viscous Protoplanetary Disks

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• Particle transport in evolving protoplanetary disks: Implications for results from Stardust
• Photophoretic separation of metals and silicates: the formation of Mercury like planets and metal depletion in chondrites
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• Collapse of a molecular cloud core to stellar densities: the radiative impact of stellar core formation on the circumstellar disc
• Thermophysical evolution of planetesimals in the Primordial Disk
• Understanding planet formation using microgravity experiments
• Three intermediate-mass YSOs with different properties emerging from the same natal cloud in IRAS 00117+6412
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Radial transport of refractory inclusions and their preservation in the dead zone
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse