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. Author manuscript; available in PMC: 2016 Jul 19.
Published in final edited form as: Geochim Cosmochim Acta. 2016 Mar 1;176:295–315. doi: 10.1016/j.gca.2015.10.036

Fig. 10.

Fig. 10

Schematic disk model (not to scale) illustrating the proposed planetesimal formation scenario in the solar protoplanetary disk. In the first few 105 years after formation of the proto-Sun, the inner disk is hot (>500 K) and characterized by early (<0.25 Myr) and rapid planetesimal formation. These planetesimals (Fig. 7), such as the Main Group Pallasite parent body (PB), form from non-carbonaceous disk material characterized by a reduced initial (26Al/27Al)0 of 1−2 × 10−5 relative to the ‘canonical’ value and deficiencies in ε54Cr. Planetesimal formation in the outer disk (Eagle Station/CV parent body) is characterized by prolonged accretion timescales from carbonaceous disk material with initial (26Al/27Al)0 of >2.7 × 10−5 and excesses in ε54Cr.