Supernova dust formation and the grain growth in the early universe: the critical metallicity for low-mass star formation. Issue 3 (28th November 2014)

• Record Type: Journal Article
• Authors: Chiaki, Gen; Marassi, Stefania; Nozawa, Takaya; Yoshida, Naoki; Schneider, Raffaella; Omukai, Kazuyuki; Limongi, Marco; Chieffi, Alessandro
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 446:Issue 3(2015)
• Page Start: 2659
• Page End: 2672
• Publication Date: 2014-11-28
• Subjects: stars: formation -- stars: low-mass -- stars: Population II -- ISM: abundances -- dust, extinction -- galaxies: evolution; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stu2298
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We investigate the condition for the formation of low-mass second-generation stars in the early Universe. It has been proposed that gas cooling by dust thermal emission can trigger fragmentation of a low-metallicity star-forming gas cloud. In order to determine the critical condition in which dust cooling induces the formation of low-mass stars, we follow the thermal evolution of a collapsing cloud by a one-zone semi-analytic collapse model. Earlier studies assume the dust amount in the local Universe, where all refractory elements are depleted on to grains, and/or assume the constant dust amount during gas collapse. In this paper, we employ the models of dust formation and destruction in early supernovae to derive the realistic dust compositions and size distributions for multiple species as the initial conditions of our collapse calculations. We also follow accretion of heavy elements in the gas phase on to dust grains, i.e. grain growth, during gas contraction. We find that grain growth well alters the fragmentation property of the clouds. The critical conditions can be written by the gas metallicity Z cr and the initial depletion efficiency f dep, 0 of gas-phase metal on to grains, or dust-to-metal mass ratio, as ( Z cr /10 −5.5 Z⊙ ) = ( f dep, 0 /0.18) −0.44 with small scatters in the range of Z cr = [0.06–3.2] × 10 −5 Z⊙ . We also show that the initial dust composition and size distribution are important to determine Z cr .