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

Klessen, Ralf S., Glover, Simon C. O. and Clark, Paul ORCID: 2012. On the formation of very metal poor stars: the case of SDSS J1029151+172927. Monthly Notices of the Royal Astronomical Society 421 (4) , pp. 3217-3221. 10.1111/j.1365-2966.2012.20544.x

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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.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: stars: abundances; stars: formation; stars: luminosity; function, mass function; stars: Population II; stars: Population III early Universe
Publisher: Oxford University Press
ISSN: 0035-8711
Last Modified: 25 Oct 2022 09:43

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