Dust Destruction in the High‐Velocity Shocks Driven by Supernovae in the Early Universe

Nozawa, Takaya; Kozasa, Takashi; Habe, Asao

doi:10.1086/505639

Cited by 161 publications

(279 citation statements)

References 73 publications

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“…Here we assume that dust grains formed at a given position distribute homogeneously within the corresponding mesh. The bulk density ρ j of each dust species is taken from Table 2 in Nozawa et al (2006), and the optical constants for calculating κ ext λ,j are taken from the references summarized in Section 4.1 in Nozawa et al (2010). 6 Note that the optical depths scale as τ λ ∝ t −2 for the free expansion of the ejecta.…”

Section: Optical Depth By Newly Formed Dustmentioning

confidence: 99%

FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE

Nozawa

Maeda

Kozasa

et al. 2011

ApJ

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We investigate the formation of dust grains in the ejecta of Type Ia supernovae (SNe Ia), adopting the carbondeflagration W7 model. In the calculations of dust formation, we apply the nucleation and grain growth theory and consider the two extreme cases of the formation of CO and SiO molecules: complete formation and no formation. The results of the calculations show that for the sticking probability of α j = 1, C, silicate, Si, and FeS grains can condense at early times of ∼100-300 days after the explosion, whereas Fe and SiC grains cannot form substantially. Due to the low gas density in SNe Ia with no H-envelope, the average radii of the newly formed grains are generally below 0.01 μm, being much smaller than those in Type II-P SNe. This supports our previous conclusion that the radius of dust formed in the ejecta is smaller in SNe with less massive envelopes. The total dust mass ranges from 3 × 10 −4 M to 0.2 M for α j = 0.1-1, depending on whether or not CO and SiO molecules are formed. We also estimate the optical depths and thermal emission by the newly formed dust and compare them to the relevant observations of SNe Ia. We find that the formation of C grains in SNe Ia must be suppressed to be consistent with observational constraints. This implies that energetic photons and electrons heavily depress the formation efficiency of C grains or that the outermost C-O layer of SNe Ia is almost fully burned. Finally, we calculate dust destruction in the SN remnants and find that dust grains formed in the ejecta of SNe Ia are almost completely destroyed in the shocked gas before being injected into the interstellar medium. This indicates that SNe Ia are unlikely to be the major sources of interstellar dust.

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Section: Optical Depth By Newly Formed Dustmentioning

confidence: 99%

FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE

Nozawa

Maeda

Kozasa

et al. 2011

ApJ

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“…The pre-shock grain size distribution is taken from the dust model of Weingartner & Draine (2001), which consists of separate carbonaceous and silicate grain populations. We now use improved sputtering yields from Nozawa et al (2006), but with a yield enhancement for small grains discussed by Jurac et al (1998). The most critical change in the model is that we now include grain motions, which result in "nonthermal sputtering" of the grains, and become important at the relatively low plasma temperatures present in the Cygnus Loop shock.…”

Section: Dust Destruction Modelsmentioning

confidence: 99%

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

Sankrit

Williams

Borkowski

et al. 2010

ApJ

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We present 24 μm and 70 μm images of a non-radiative shock in the Cygnus Loop supernova remnant, obtained with the Multiband Imaging Photometer for Spitzer on board the Spitzer Space Telescope. The post-shock region is resolved in these images. The ratio of the 70 μm to the 24 μm flux rises from about 14 at a distance 0. 1 behind the shock front to about 22 in a zone 0. 75 further downstream, as grains are destroyed in the hot plasma. Models of dust emission and destruction using post-shock electron temperatures between 0.15 keV and 0.30 keV and post-shock densities, n H ∼ 2.0 cm −3 , predict flux ratios that match the observations. Non-thermal sputtering (i.e., sputtering due to bulk motion of the grains relative to the gas) contributes significantly to the dust destruction under these shock conditions. From the model calculations, we infer that about 35% by mass of the grains are destroyed over a 0.14 pc region behind the shock front.

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“…The Mixed progenitor model gives a bigger upper limit for the grain size. Since the gain population still needs to cross the reverse shock, where the smallest grains are likely to be destroyed by sputtering (Nozawa et al 2006;Bianchi & Schneider 2007), the small differences seen here could be much more substantial when the dust is recycled into the interstellar medium.…”

Section: Resultsmentioning

confidence: 93%

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

Lazzati

Heger

2016

ApJ

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Core-collapse supernovae (CCSNe) are considered to be important contributors to the primitive dust enrichment of the interstellar medium in the high-redshift universe. Theoretical models of dust formation in stellar explosions have so far provided controversial results and a generally poor fit to the observations of dust formation in local supernovae. We present a new methodology for the calculation of carbonaceous dust formation in young supernova remnants. Our new technique uses both the nucleation theory and a chemical reaction network to allow us to compute the dust growth beyond the molecular level as well as consider the chemical erosion of the forming grains. We find that carbonaceous dust forms efficiently in the core of the ejecta, but takes several years to condensate, longer than previously estimated. It forms unevenly and remains concentrated in the inner part of the remnant. These results support the role of CCSNe as dust factories and provide new insight into the observations of SN1987A, in which large amounts of dust have been detected to form on a timescale of years after core-collapse.

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Dust Destruction in the High‐Velocity Shocks Driven by Supernovae in the Early Universe

Cited by 161 publications

References 73 publications

FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE

FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

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

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