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• W2026422443 abstract "We show that the explosion of the first supernovae can trigger low-mass star formation via gravitational fragmentation of the supernova-driven gas shell. If the shell mass does not exceed the host galaxy gas mass, all explosions with energies ESN⩾1051 erg can lead to shell fragmentation. However, the minimum ambient density required to induce such fragmentation is much larger, n0>300 cm−3, for Type II supernovae than for pair-instability ones, which can induce star formation even at lower ambient densities. The typical mass of the unstable fragments is ∼104−7M⊙; their density is in the range 110–6×107 cm−3. Fragments have a metallicity strictly lower than 10−2.6Z⊙ and large values of the gravitational-to-pressure force ratio f≃8. Based on these findings, we conclude that the second generation of stars produced by such self-propagating star formation is predominantly constituted by low-mass, long-living, extremely metal-poor (or even metal-free, if mixing is suppressed) stars. We discuss the implications of such results for Pop III star formation scenarios and for the most iron-poor halo star HE0107-5240." @default.
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• W2026422443 date "2004-12-01" @default.
• W2026422443 modified "2023-10-01" @default.
• W2026422443 title "Induced formation of primordial low-mass stars" @default.
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• W2026422443 doi "https://doi.org/10.1016/j.newast.2004.06.003" @default.
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