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

By T. Nozawa, T. Kozasa, H. Umeda, K. Maeda, K. Nomoto. 2003

332 citations recorded by the source corpus.

Dust grains play a crucial role in the 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 progenitor mass Mpr ranging from 13 to 30 M☉ and for pair-instability supernovae with Mpr = 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 radioactive 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 follows: 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 a range of 3 orders of magnitude, depending on the grain species and the formation condition, and the maximum radius is limited to less than 1 μm, which does not depend on the progenitor mass. The size distribution function of each grain species is approximately lognormal, except for Mg silicates, MgO, Si, and FeS in the unmixed case and Al2O3 in both cases. The size distribution function summed up over all grain species is approximated by a power-law formula whose index is -3.5 for the larger radius and -2.5 for the smaller one; the radius at the crossover point ranges from 0.004 to 0.1 μm, depending on the model of supernovae. The fraction of mass locked into dust grains increases with increasing the progenitor mass: 2%-5% of the progenitor mass for core-collapse supernovae and 15%-30% for pair-instability supernovae whose progenitor mass ranges from 140 to 260 M☉. Thus, if very massive stars populated the first generation of stars (Population III stars), a large amount of dust grains would be produced in the early universe. We also discuss the dependence of the explosion energy and the amount of 56Ni in the ejecta, as well as the efficiency of formation of CO and SiO molecules, on the formation of dust grains in the ejecta of supernovae.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/19e9b5ba9acdd32e1a2316b13c2257db4b4a3c83

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Citations in the corpus

The First Stars (2003, background): “The physical nature of the dust, however, that is produced by the first SNe is currently still rather uncertain (e.g., Loeb & Haiman 1997, Todini & Ferrara 2001, Nozawa et al. 2003, Schneider et al. 2003b).”
Dust formation and survival in supernova ejecta (2007, methodology): “The procedure is analogous to that adopted by Hirashita et al. (2005) when modelling the dust extinction from the SNe dust models of Nozawa et al. (2003).”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “Observations are inconclusive and the theory is only in its infancy (Schneider et al. 2004; Nozawa et al. 2003, and references therein).”
Fragmentation of star-forming clouds enriched with the first dust (2006, background): “Theoretical models suggest that a significant fraction of these heavy elements could be in the form of dust grains (Kozasa, Hasegawa & Nomoto 1989; Todini & Ferrara 2001; Nozawa et al. 2003; Schneider, Ferrara & Salvaterra 2004).”
DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj (2009, background): “Moreover, both Todini & Ferrara (2001) and Nozawa et al. (2003) find carbon dust condensation is complete in not much more than one year.”
The First Cosmic Structures and Their Effects (2004, background): “These conclusions depend very weakly on the thermodynamics of the ejecta, which instead affect considerably the grain formation epoch, composition and size distribution (Nozawa et al. 2003).”
Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium (2012, background): “Dust grains not only originate from stars, but are also destroyed by SNe blast waves (e.g., Jones et al., 1994, 1996; Nozawa et al., 2003; Zhukovska et al., 2008).”
The transition from population III to population II-I star formation (2010, background): “…updated value of Z⊙ ≃ 0.0134 mass of SNII/PISN progenitor, reaches2% − 5% of the parent mass for type-II SN (Kozasa et al. 1991; Todini & Ferrara 2001; Nozawa et al. 2003; Bianchi & Schneider 2007), and15% − 30% for PISN (Nozawa et al. 2003; Schneider et al. 2004), in a few hundred days after…”
The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of a Strongly Magnetized Neutron Star (2007, background): “The temperature in the ejecta at t ∼ 50d should be too high to form dust in the ejecta (e.g., Nozawa et al. 2003).”
Thermal and Fragmentation Properties of Star-forming Clouds in Low-Metallicity Environments (2005, background): “Also, the elemental abundance ratios in ejecta from the first SNe are different from those in local ISM,whichwe have used in the analysis in this paper.”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “…the availability of metals, dust formation (and in turn, subsequent dust cooling) became possible (e.g., in supernova ejecta; Todini & Ferrara 2001, Nozawa et al. 2003, Schneider, Ferrara & Salvaterra 2004, Omukai et al. 2005, Cherchneff & Dwek 2010, Schneider et al. 2012a, Klessen, Glover &…”
Production of dust by massive stars at high redshift (2011, background): “Consequently, several theoretical models for dust formation in CCSNe have been developed, which result in dust masses of up to 1 M⊙ per SN within the first∼600 days after the explosion (e.g., Kozasa et al, 1989, 1991; Clayton et al, 1999, 2001; Todini and Ferrara, 2001; Nozawa et al, 2003).”
Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by the Spitzer Space Telescope (2007, background): “Theoretical studies (Kozasa et al. 1991; Todini & Ferrara 2001, hereafter TF01; Nozawa et al. 2003, hereafter N03) predicted the formation of a significant quantity of dust ( 0:1Y1:0 M ) in the ejecta of Type II SNe, and the predicted dust mass is believed to be sufficient to account for the quantit”
The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, methodology): “We take the dust particle size to be 0.1µm and density to be 2.5g/cc (Todini & Ferrara 2001; Nozawa et al. 2003).”
Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and Be Injected into the Early Interstellar Medium? (2007, methodology): “Theoretical studies aimed at determining the composition and yield of dust in the ejecta of primordial Type II SNe (SNe II) and pair-instability SNe (PISNe) were conducted by Todini & Ferrara (2001), Nozawa et al. (2003), and Schneider et al. (2004).”
Stellar sources of dust in the high-redshift Universe (2009, methodology): “The former class is predicted tobe the end-product of the evolution of very massive Population IIIstars with masses in the range 140M⊙ 6 M 6 260M⊙ and might provide an important source of dust at high redshift (Schneider, Ferrara & Salvaterra 2004; Nozawa et al. 2003).”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “Interstellar dust is produced in the ejecta of asymptotic giant branch (AGB) stars and supernovae (SNe, Gehrz 1989; Todini & Ferrara 2001; Nozawa et al. 2003; Ferrarotti & ?”
DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA (2013, background): “(Todini & Ferrara 2001; Nozawa et al. 2003; Cherchneff & Dwek 2010).”
The First Stellar Cluster (2007, methodology): “However, the use of this alternative dust model can also be questioned, since Nozawa et al. (2003) have shown that the composition and properties of the dust produced by population III supernovae are strongly dependent on the (poorly-constrained) degree of mixing assumed to occur in the ejecta, and…”