Dust Formation in Primordial Type II Supernovae

By P. Ferrara. 2000

437 citations recorded by the source corpus.

We have investigated the formation of dust in the ejecta of Type II supernovae (SNe), mostly of primordial composition, to answer the question of where are the first solid particles formed in the universe. However, we have also considered non-zero progenitor’s metallicity values up to Z = Z⊙. The calculations are based on standard nucleation theory and the scheme has been first tested on the well studied case of SN1987A, yielding results that are in agreement with the available data. We find that: i) the first dust grains are predominantly made of silicates, amorphous carbon (AC), magnetite, and corundum; ii) the largest grains are the AC ones, with sizes around 300u , whereas other grain types have smaller radii, around 10-20u The grain size distribution depends somewhat on the thermodynamics of the ejecta expansion and variations in the results by a factor � 2 might occur within reasonable estimates of the relevant parameters. Also, and for the same reason, the grain size distribution, is essentially unaffected by metallicity changes. The predictions on the amount of dust formed are very robust: for Z = 0, we find that SNe with masses in the range (12-35)M⊙ produce about 0.08M⊙ < Md < � 0.3M⊙ of dust/SN. The above range increases by roughly 3 times as the metallicity is increased to solar values. We discuss the implications and the cosmological consequences of the results.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b2578193eaeb4ab95a51ac6c7448c7c71f0bf001

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Citations in the corpus

• 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).”
• 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).”
• On the Maximum Luminosity of Galaxies and Their Central Black Holes: Feedback from Momentum-driven Winds (2004, background): “Instead, Kozasa et al. (1989), Todini & Ferrara (2001), and Nozawa et al. (2003) show that supernovae can produceMDust∼ 0.5 M⊙ of dust per supernova, depending on the progenitor metallicity and mass.”
• DUST OBSCURATION AND METALLICITY AT HIGH REDSHIFT: NEW INFERENCES FROM UV, Hα, AND 8 μm OBSERVATIONS OF z ∼ 2 STAR-FORMING GALAXIES (2010, background): “In this case, the mid-IR emission observed in the young galaxies may be due to some combination of silicate and amorphous carbon dust produced in Type II supernovae (Todini & Ferrara 2001).”
• 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).”
• The Absence of Crystalline Silicates in the Diffuse Interstellar Medium (2004, methodology): “The authors have derived this rate by scaling the dust production rates for type II supernovae (Todini & Ferrara 2001) with the dust condensation efficiency determined for Cas A, assuming it had a 30 M progenitor, and applying a supernova rate, which arises from standard values of the initial mass…”
• ON THE STELLAR POPULATIONS AND EVOLUTION OF STAR-FORMING GALAXIES AT 6.3 < z ⩽ 8.6 (2009, background): “Todini & Ferrara (2001) show that∼ 0.1– 0.3 M⊙ of dust form per star with initial masses of 12–35 M⊙, which end as SNe after 20 Myr.”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “The expectation of rapid dust enrichment from core-collapse supernovae (Todini & Ferrara 2001) implies that it is unlikely that the dust obscuration can be significantly lower than this value when observed for dynamically-relaxed systems.”
• On the properties of massive Population III stars and metal-free stellar populations (2001, background): “Important advances have been made in recent years on the modeling of the first stars and galaxies forming out of pristine matter — so called Population III (Pop III) objects — in the early Universe (see e.g. the proceedings of Weiss et al. 2000 and Umemura & Susa 2001).”
• The First Stellar Cluster (2007, methodology): “Schneider et al. (2006) have performed a similar study to that of Omukai et al. (2005), but use a dust model based on the results of Todini & Ferrara (2001) and Schneider, Ferrara, & Salvaterra (2004) in place of the Pollack et al. (1994) dust model.”
• Dust formation in early galaxies (2003, background): “Others however, propose that supernovae explosions must be an important contributor to dust formation (Dwek & Scalo 1980, Todini & Ferrara 2001 (hereafter TF01)) to account for the dust observed at high redshifts (as seen in Damped Lyman Alpha systems and in SCUBA data (Frayer & Scoville 1999)).”
• Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “With 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 &…”
• Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae (2003, methodology): “Todini & Ferrara (2001) performed dust formation calculations in primordial corecollapse supernovae (CCSNe) with progenitor mass Mpr ranging from 12 to 35 M , adopting the models of supernovae byWoosley &Weaver (1995) and applying themethod of dust formation calculation for SN 1987A by Kozasa et…”
• Star Formation at Very Low Metallicity. I. Chemistry and Cooling at Low Densities (2007, background): “…be to adopt a grain-size distribution and mix of compositions based on the results of numerical modeling of dust formation in highredshift supernovae (Todini & Ferrara 2001; Nozawa et al. 2003; Schneider et al. 2004) and then to compute the H2 formation rate expected for this grain population.”
• THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “They are responsible for the majority of heavy elements (e.g., Matteucci & Greggio 1986), are associated with dust production (e.g., Todini & Ferrara 2001), and could dominate winds and feedback in galaxy formation (e.g., Ferrara & Ricotti 2006).”
• Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “From the theoretical side also, little is known about dust condensation in SNe; only a few model calculations for dust condensation in super-nova ejecta are available (Kozasa et al. 1989; Todini & Ferrara 2001; Nozawa et al. 2003; Schneider et al. 2004), and they are of a very qualitative nature.”
• DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA (2013, background): “(Todini & Ferrara 2001; Nozawa et al. 2003; Cherchneff & Dwek 2010).”