From Dust to Terrestrial Planets – Introduction |
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Authors: | Reinald Kallenbach Willy Benz Günter W Lugmair |
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Institution: | 1. International Space Science Institute, CH-3012, Bern, Switzerland 2. Physikalisches Institut der Universit?t Bern, CH-3012, Bern, Switzerland 3. Max-Planck-Institut für Chemie, Kosmochemie, D-55020, Mainz, Germany
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Abstract: | Terrestrial planets are accreted in a disk orbiting a central star. The basic challenge of their formation consists of assembling
micron-sized or smaller dust grains to bodies with over 104 km in diameter. This formation process, ultimately based on collisions, occurs in three very different physical regimes depending
upon the size of the bodies present: 1) Early on, micron- to mm-sized dust grains, chondrules and chondrites are strongly
coupled to the gas. 2) As they grow larger, gravity increases the collisional cross section allowing runaway growth to occur.
3) After this runaway phase stops from exhaustion of matter in the immediate surroundings of the protoplanets, further growth
occurs on timescales typical of mutual gravitational perturbations. The emphasis of this book is on the timescales corresponding
to these formation phases as well as the characteristic chemical and isotopic composition of the bodies involved.
This revised version was published online in June 2006 with corrections to the Cover Date. |
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