Are the Formation and Abundances of Metal-poor Stars the Result of Dust Dynamics?

作者：Hopkins Philip F; Conroy Charlie

来源：Astrophysical Journal, 2017, 835(2): 154.

DOI：10.3847/1538-4357/835/2/154

• dark ages,reionization,first stars
• galaxies: formation
• galaxies: star formation
• stars: abundances
• stars: formation
• turbulence

Large dust grains can fluctuate dramatically in their local density, relative to the gas, in neutral. turbulent disks. Small, high-redshift galaxies (before reionization) represent ideal environments for this process. We show via simple arguments and simulations that order-of-magnitude fluctuations are expected in local abundances of large grains (>100 angstrom) under these conditions. This can have important consequences for star formation and stellar metal abundances in extremely metal-poor stars. Low-mass stars can. form in dust-enhanced regions almost immediately after some dust forms. even if the galaxy-average metallicity is too low for fragmentation to occur. We argue that the metal abundances of these "promoted" stars may contain interesting signatures. as the CNO abundances (concentrated in large carbonaceous grains and ices) and Mg and Si (in large silicate grains) can be enhanced and/or fluctuate almost independently. Remarkably, the otherwise puzzling abundance patterns of some metal-poor stars can be well. fit by standard. IMF-averaged core-collapse SNe yields. if we allow for fluctuating local dust-to-gas ratios. We also show that the observed log-normal. distribution of enhancements in these species agrees with our simulations. Moreover, we confirm that Mg and Si are correlated in these stars;. the. abundance ratios are similar to those in local silicate grains. Meanwhile [Mg/Ca], predicted to be nearly invariant from pure SNe yields, shows very large enhancements and variations up to factors of greater than or similar to 100 as expected in the dust-promoted model, preferentially in the [C/Fe]-enhanced metal-poor stars. Together, this suggests that (1) dust exists in second-generation star formation, (2) local dust-to-gas ratio fluctuations occur in. protogalaxies and can be important for star formation, and (3) the light element abundances of these stars may be affected by the local chemistry of dust where they formed, rather than directly tracing nucleosynthesis from earlier populations.

• 出版日期2017-2-1