Star Formation in a Low-Metallicity Gas

Details Star Formation in a Low-Metallicity Gas Star Formation in a Low-Metallicity Gas

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1294..297y&link_type=abstract

THE FIRST STARS AND GALAXIES: CHALLENGES FOR THE NEXT DECADE. AIP Conference Proceedings, Volume 1294, pp. 297-298 (2010).

Physics

Star Formation, Radiative Transfer, Hydrogen, Star Formation, Radiative Transfer, Scattering, Hi Regions And 21-Cm Lines, Diffuse, Translucent, And High-Velocity Clouds

Scientific paper

We present high resolution simulations of star formation in a low-metallicity gas. Our models include relevant chemical and radiative processes in a direct, self-consistent manner. In particular, we calculate radiative transfer and the resulting cooling by thermal emission by dust. We show that vigorous fragmentation is triggered in a star-forming gas at a metallicity as low as [Z/H]~-5. Dust cooling at high densities, rather than line cooling by carbon or oxygen atoms, is responsible for the rapid cooling and fragmentation.

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