Journal Article

On the formation of very metal poor stars: the case of SDSS J1029151+172927

Ralf S. Klessen, Simon C. O. Glover and Paul C. Clark

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 421, issue 4, pages 3217-3221
Published in print April 2012 | ISSN: 0035-8711
Published online April 2012 | e-ISSN: 1365-2966 | DOI:
On the formation of very metal poor stars: the case of SDSS J1029151+172927

Show Summary Details


The formation of stars is a key process in the early universe with far‐reaching consequences for further cosmic evolution. While stars forming from truly primordial gas are thought to be considerably more massive than our Sun, stars in the universe today have typical masses below one solar mass. The physical origin of this transition and the conditions under which it occurs are highly debated. There are two competing models: one based on metal‐line cooling as the primary agent and one based on dust cooling. The recent discovery of the extremely metal poor star SDSS J1029151+172927 provides a unique opportunity to distinguish between these two models. Based on simple thermodynamic considerations we argue that SDSS J1029151+172927 was more likely formed as a result of dust continuum cooling rather than cooling by metal lines. We conclude that the masses of extremely metal poor stars are determined by dust‐induced fragmentation.

Keywords: stars: abundances; stars: formation; stars: luminosity function, mass function; stars: Population II; stars: Population III; early Universe

Journal Article.  3799 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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