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We investigate the radiativetransport of dust inprimordial galaxies in thepresence of the UVradiation field from thefirst metal-free stars. Wefind that dust createdin the first supernova(SN) explosions can bedriven through the interiorof the SN remnantto accumulate in theSN shells, where second-generationstars may form fromcompressed cooling gas. Thisscenario requires metal-free starsto form continuously overtimescales of up to10 Myr, consistent withrecent estimates. Silicate andgraphite grains, as wellas iron-bearing magnetites, aretransported to the shellsfor reasonable parameter assumptions,but their relative yieldsfrom primordial SNe isan important factor inthe resulting abundance ratios.We compare the resultsof segregated grain transportwith the current nucleosyntheticdata on extremely metal-poorGalactic halo stars. Fossilsignatures of this processmay already have beendetected in those iron-poorstars with enhanced carbonand silicate elements suchas magnesium, silicon andoxygen. We discuss theimplications of our resultsfor the transition fromfirst- to second-generation starformation in primordial galaxies,and the role playedby the radiative transportof dust in thisprocess.


Copyright 2006 American Astronomical Society.

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