Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and Be Injected into the Early Interstellar Medium?

By T. Nozawa, T. Kozasa, A. Habe, E. Dwek, H. Umeda, Nozomu Tominaga, K. Maeda, Ken'ichi Nomoto. 2007

232 citations recorded by the source corpus.

We investigate the evolution of dust that formed at Population III supernova (SN) explosions and its processing through the collisions with the reverse shocks resulting from the interaction of the SN ejecta with the ambient medium. In particular, we investigate the transport of the shocked dust within the SNR and its effect on the chemical composition, the size distribution, and the total mass of dust surviving in SNRs. We find that the evolution of the reverse shock, and hence its effect on the processing of the dust, depends on the thickness of the envelope retained by the progenitor star. Furthermore, the transport and survival of the dust grains depend on their initial radius, aini, and composition: for Type II SNRs expanding into the ISM with a density of nH,0 = 1 cm-3, small grains with aini ≲ 0.05 μm are completely destroyed by sputtering in the postshock flow, while grains with aini = 0.05-0.2 μm are trapped into the dense shell behind the forward shock. Very large grains of aini ≳ 0.2 μm are ejected into the ISM without decreasing their sizes significantly. We find that the total mass fraction of dust that is destroyed by the reverse shock ranges from 0.2 to 1.0, depending on the energy of the explosion and the density of the ambient ISM. The results of our calculations have significant impact on the abundance pattern of the second-generation stars that form in the dense shell of primordial SNRs.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fc695ab2be1f42195e93eb53317df67d40b816b2

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Citations in the corpus

The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “…systems are characterized by a small content of dust (which should reprocess UV light into IR thermal emission), both because of their low metallicity and because of shortage of time to produce dust (Valiante et al. 2009, 2011; Schneider et al. 2014; Hirashita et al. 2014; Nozawa et al. 2007).”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “E-mail: gpopping@eso.org Gail 2006; Nozawa et al. 2007; Zhukovska, Gail & Trieloff 2008; Nanni et al. 2013).”
DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA (2013, background): “Models of dust destruction predict a wide range of survival fractions (Nozawa et al. 2007).”
Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by the Spitzer Space Telescope (2007, background): “…by the reverse shock is highly dependent on the thickness of the hydrogen envelope at the time of explosion and that the evolution and destruction of dust grains formed in SNe strongly depend not only on their initial sizes but also the density of ambient interstellar medium (Nozawa et al. 2007).”
Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium (2012, background): “The importance of large grains is further enhanced given that the grain size distribution tends to be biased to large (a ∼ 0.1 µm) size by the destruction within SN remnants (Nozawa et al., 2007).”
Stellar sources of dust in the high-redshift Universe (2009, methodology): “This is at odd with the models developed by Nozawa et al. (2003, 2007), in which the composition is dominated by silicate and iron grains.”
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).”
Astrophysics with Extraterrestrial Materials (2016, background): “Many studies indicate that the timescale for dust destruction in the ISM is much shorter than the timescale of injection of fresh stardust, and this is commonly taken to mean that much of the observed dust forms directly in the ISM (Draine 1990, 2009).”
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).”