Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011dda....42.0907h&link_type=abstract
American Astronomical Society, DDA meeting #42, #9.07; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
It has been suggested by Bottke et al (2006) that the extraordinary number of different parent bodies of iron meteorite, and the dearth of asteroids and meteorites derived from the silicate mantles and crusts of these objects, could be better understood if these bodies accreted rapidly at 1-2 AU during the first 1.5 Myr when 26Al melted all ice-free planetesimals larger than 20 km in radius. These authors proposed that planetary embryos at 1-2 AU dynamically excited the differentiated planetesimals and scattered their fragments into the asteroid belt where they were captured by embryos in that region. As part of our on-going project on understanding the details of this process, we have simulated the dynamics of a disk of planetesimals and planetary embryos in the region between 0.5 and 4 AU for different radial dependence of disk's surface density profile. We have considered disks with radial profiles of -0.5, -1, and -1.5, and simulated the collision and accretion of planetesimals and planetary embryos with and without giant planets. Results indicate that the out-scattering of planetesimals from the region of 1-2 AU to the inner asteroid belt is more efficient for disk surface density profiles that are less steep. The timescale for the delivery of differentiated planetesimals to the inner asteroid belt also varies with the radial dependence of the disk surface density. We present the results of our simulations and discuss their implications for the origin of the parent bodies of iron meteorites.
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