Volume 504, Number 1, September II 2009
|Page(s)||109 - 113|
|Section||Interstellar and circumstellar matter|
|Published online||09 July 2009|
Protostellar collapse: rotation and disk formation
Zentrum für Astronomie (ZAH), Institut für Theoretische Astrophysik (ITA), Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany e-mail: firstname.lastname@example.org
2 Institut für Geowissenschaften, Universität Heidelberg, Im Neuenheimer Feld 236, 69120 Heidelberg, Germany
Accepted: 8 June 2009
We present some important conclusions from models of the collapse of rotating molecular cloud cores with axial symmetry, corresponding to the evolution of young stellar objects from class 0 to the beginning of class I. There are three main findings of the calculations: (1) the typical timescale for building up a preplanetary disk, which was found to be of the order of one free-fall time 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 causing the growing disk to become more stable and strengthening the intrinsic meridional circulation pattern of the accretion flow; and (3) the origin of calcium-aluminium-rich inclusions (CAIs). Because of the persistent equatorial outflow, material that has undergone substantial chemical and mineralogical modifications in the hot (900 K) interior of the protostellar core may have a good chance of being advectively transported outward into the cooler remote parts (4 AU, say) of the growing disk and surviving there until it is incorporated into a meteoritic parent body.
Key words: stars: formation / accretion, accretion disks / planetary systems: formation
© ESO, 2009
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