Dust formation and survival in supernova ejecta

By Simone Bianchi, Raffaella Schneider. 2007

330 citations recorded by the source corpus.

The presence of dust at high redshift requires efficient condensation of grains in SN ejecta, in accordance with current theoretical models. Yet, observations of the few well studied SNe and SN remnants imply condensation efficiencies which are about two orders of magnitude smaller. Motivated by this tension, we have (i) revisited the model of Todini & Ferrara (2001) for dust formation in the ejecta of core collapse SNe and (ii) followed, for the first time, the evolution of newly condensed grains from the time of formation to their survival - through the passage of the reverse shock - in the SN remnant. We find that 0.1 - 0.6 M⊙ of dust form in the ejecta of 12 - 40 M⊙ stellar progenitors. Depending on the density of the surrounding ISM, between 2-20% of the initial dust mass survives the passage of the reverse shock, on time-scales of about 4 8×10 4 yr from the stellar explosion. Sputtering by the hot gas induces a shift of the dust size distribution towards smaller grains. The resulting dust extinction curve shows a good agreement with that derived by observations of a reddened QSO at z = 6.2. Stochastic heating of small grains leads to a wide distribution of dust temperatures. This supports the idea that large amounts (� 0.1M⊙) of cold dust (T � 40K) can be present in SN remnants, without being in conflict with the observed IR emission.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/671bd0ae7a335fe54a9b439e4e47747809ee16ef

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Citations in the corpus

The UV continua and inferred stellar populations of galaxies at z ~7-9 revealed by the Hubble Ultra-Deep Field 2012 campaign (2012, methodology): “…β values derived by repeating the at U niversity of St A ndrew s on A ugust 13, 2014 http://m nras.oxfordjournals.org/ D ow nloaded from 3530 J. S. Dunlop et al. power-law fitting after taking into account the dust enrichment and applying the SN extinction curve (Bianchi & Schneider 2007).”
Production of dust by massive stars at high redshift (2011, methodology): “Similar to the study of Bianchi and Schneider (2007), Nozawaet l (2007) investigate dust destruction caused by the impact of the reverse shock inthe SNR phase of zero metallicity stars.”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “The dust ﬁrst formed in the expanding SN ejecta is later overrun by the reverse shock and part of it is destroyed again (Dwek 2005; Bianchi & Schneider 2007; Nozawa et al. 2007).”
Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies? (2008, background): “However, their composition and size distribution are still affected by many uncertainties, such as the degree of mixing in the ejecta and the efficiency of grain condensation and their destruction by the reverse shock (Nozawa et al. 2007; Bianchi & Schneider 2007).”
Stellar sources of dust in the high-redshift Universe (2009, methodology): “It is worth noting that the model by Bianchi & Schneider (2007) shows that SNe are expected to produce mainly carbon, magnetite and corundum grains.”
Star Formation at Very Low Metallicity. I. Chemistry and Cooling at Low Densities (2007, background): “In addition, the effects of dust destruction in the supernova reverse shock remain uncertain (Bianchi & Schneider 2007; Nozawa et al. 2007).”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, background): “If core-collapse SNe are not significant producers of dust (e.g. Barlow et al. 2010) or if most of their dust is then destroyed in the remnant (Bianchi & Schneider 2007) then this fraction decreases to χ 1 ≤ 0.1, making it difficult to explain the dust masses we see in our Galaxy or in…”
Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium (2012, background): “Furthermore, Calura et al. (2008) have shown that the dust destruction rate by SNe Ia is about 1/10 of that by SNe II.”
Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and Be Injected into the Early Interstellar Medium? (2007, background): “Recently, Bianchi & Schneider (2007) have studied the evolution of newly condensed grains through the passage of the reverse shock by using a semianalytical model and have showed that the fraction of dust mass survived ranges between 2% and 20%depending on the density in the ISM.”
The First Stellar Cluster (2007, background): “…ejecta, and since the model does not take into account the destruction of grains by thermal sputtering in the reverse shock in the supernova remnant (Bianchi & Schneider 2007), or the growth of grains through accretion or coagulation during the protostellar collapse (see e.g. Flower et al. 2005).”
The transition from population III to population II-I star formation (2010, background): “…≃ 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 beginning of the…”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “Besides theoretical work on the condensation efficiency of AGB stars and SNe (Ferrarotti & Gail 2006; Bianchi & Schneider 2007), our predicted dust abundances also suggest that constant high condensation efficiencies (as in e.g., Bekki 2013; McKinnon et al. 2016) are an unrealistic way of building…”
simba: Cosmological simulations with black hole growth and feedback (2019, methodology): “Guided by computations of Bianchi & Schneider (2007), we choose the dust condensation efficiency of Type II SNe δSNII i,dust = 0.15 to match the low-metallicity end of the observed relation between dust-to-gas mass ratios (DGR) and gas-phase metallicities (Rémy-Ruyer et al. 2014).”