期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 452, 期 3, 页码 2822-2836出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv1509
关键词
hydrodynamics; radiative transfer; methods: numerical; galaxies: star formation
资金
- NSF [ACI-1238993, PHY-0941373, AST-1211626, AST-1333360]
- state of Illinois
- NSF PRAC [OCI-0832662]
- MSU Institute for Cyber-Enabled Research
- NASA [NNX12AC98G]
- Hubble Theory Grant [HST-AR-13261.01-A, HST-AR-13895.001-A]
- sabbatical visitor program at the Michigan Institute for Research in Astrophysics (MIRA) at the University of Michigan in Ann Arbor
- National Science Foundation (NSF) [AST-1109243]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1333360, 1211626] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1333514] Funding Source: National Science Foundation
We present a simulation of the formation of the earliest Population II stars, starting from cosmological initial conditions and ending when metals created in the first supernovae are incorporated into a collapsing gas cloud. This occurs after a supernova blast-wave collides with a nearby mini-halo, inducing further turbulence that efficiently mixes metals into the dense gas in the centre of the halo. The gas that first collapses has been enriched to a metallicity of Z similar to 2 x 10(-5) Z(circle dot). Due to the extremely low metallicity, collapse proceeds similarly to metal-free gas until dust cooling becomes efficient at high densities, causing the cloud to fragment into a large number of low-mass objects. This external enrichment mechanism provides a plausible origin for the most metal-poor stars observed, such as SMSS J031300.36-670839.3, that appear to have formed out of gas enriched by a single supernova. This mechanism operates on shorter time-scales than the time for low-mass mini-haloes (M <= 5 x 10(5) M-circle dot) to recover their gas after experiencing a supernova. As such, metal-enriched stars will likely form first via this channel if the conditions are right for it to occur. We identify a number of other externally enriched haloes that may form stars in this manner. These haloes have metallicities as high as 0.01 Z(circle dot), suggesting that some members of the first generation of metal-enriched stars may be hiding in plain sight in current stellar surveys.
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