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A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
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A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
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Journal Article
A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
2002
Overview
Determining the chronology for the assembly of planetary bodies in the early Solar System is essential for a complete understanding of star- and planet-formation processes. Various radionuclide chronometers (applied to meteorites) have been used to determine that basaltic lava flows on the surface of the asteroid Vesta formed within 3 million years (3 Myr) of the origin of the Solar System
1
,
2
,
3
. Such rapid formation is broadly consistent with astronomical observations of young stellar objects, which suggest that formation of planetary systems occurs within a few million years after star formation
4
,
5
. Some hafnium–tungsten isotope data, however, require that Vesta formed later
6
(∼16 Myr after the formation of the Solar System) and that the formation of the terrestrial planets took a much longer time
7
,
8
,
9
,
10
(62
-14
+4504
Myr). Here we report measurements of tungsten isotope compositions and hafnium–tungsten ratios of several meteorites. Our measurements indicate that, contrary to previous results
7
,
8
,
9
,
10
, the bulk of metal–silicate separation in the Solar System was completed within <30 Myr. These results are completely consistent with other evidence for rapid planetary formation
1
,
2
,
3
,
4
,
5
, and are also in agreement with dynamic accretion models
11
,
12
,
13
that predict a relatively short time (∼10 Myr) for the main growth stage of terrestrial planet formation.
Publisher
Nature Publishing Group UK,Nature Publishing,Nature Publishing Group
Subject
