Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae

Abstract

Dust grains play a crucial role on formation and evolution history of stars and galaxies in the early universe. We investigate the formation of dust grains in the ejecta of population III supernovae including pair-instability supernovae which are expected to occur in the early universe, applying a theory of non-steady state nucleation and grain growth. Dust formation calculations are performed for core collapse supernovae with the progenitor mass M pr ranging from 13 to 30 M ⊙ and for pair-instability supernovae with M pr = 170 and 200 M ⊙ . In the calculations, the time evolution of gas temperature in the ejecta, which strongly affects the number density and size of newly formed grains, is calculated by solving the radiative transfer equation taking account of the energy deposition of radio active elements. Two extreme cases are considered for the elemental composition in the ejecta; unmixed and uniformly mixed cases within the He-core, and formation of CO and SiO molecules is assumed to be complete.The results of calculations for core collapse supernovae and pair-instability supernovae are summarized as the followings; in the unmixed ejecta, a variety of grain species condense, reflecting the difference of the elemental composition at the formation site in the ejecta, otherwise only oxide grains condense in the uniformly mixed ejecta. The average size of newly formed grains spans the range

Classification of extremely metal-poor stars: absent region in A(C)–[Fe/H] plane and the role of dust cooling

“…We in this section show this difference in grain radius with a dust formation model. In the early Universe, dust grains are mainly supplied by supernovae (SNe) arising from first-generation metal-free (Pop III) stars (Todini & Ferrara 2001;Nozawa et al 2003). Marassi et al 2014;Tominaga et al 2014;Ishigaki et al 2014).…”

The dust content of galaxies from z = 0 to z = 9

“…Interstellar dust is produced in the ejecta of asymptotic giant branch (AGB) stars and supernovae (SNe, Gehrz 1989; E-mail: gpopping@eso.org Todini & Ferrara 2001;Nozawa et al 2003;Ferrarotti & Gail 2006;Nozawa et al 2007;Zhukovska, Gail & Trieloff 2008;Nanni et al 2013). After the initial formation, dust growth can occur in the dense ISM via accretion of metals onto dust particles (Draine 1990;Dominik & Tielens 1997;Dwek 1998;Draine 2009;Hirashita & Kuo 2011;Zhukovska 2014).…”

The Interplay Between Chemistry and Nucleation in the Formation of Carbonaceous Dust in Supernova Ejecta

“…With respect to classical calculations (Kozasa et al 1989(Kozasa et al , 1991Todini & Ferrara 2001;Nozawa et al 2003;Fallest et al 2011) and to the results of Sarangi & Cherchneff (2015), we find that our new code predicts a much more gradual carbon dust formation, beginning just a few months after the core-collapse and continuing for a few years. Despite the more gradual formation, however, we are not able to fully reproduce the observational results that require an even more gradual and continuous dust formation in the ejecta, with dust appearing as early as two months after core-collapse and gradually increasing for a few years to a decade (Gall et al 2014), eventually leading to a highly efficient condensation of a sizable fraction of a solar mass (Indebetouw et al 2014).…”

“…Calculations based on the classical nucleation theory (e.g., Feder et al 1966) typically predict the prompt formation of fairly large amounts of dust, of the order of one solar mass or more, within one year from the explosion (Kozasa et al 1989(Kozasa et al , 1991Clayton et al 2001;Todini & Ferrara 2001;Nozawa et al 2003Nozawa et al , 2010. The result is robust for the unknown parameters of the theory, such as the shape and sticking coefficients of the grains, at least to first order (Fallest et al 2011).…”