Late formation of silicon carbide in type II supernovae

Liu, Nan; Nittler, L. R.; Alexander, Conel M. O'd.; Wang, Jingyuan

doi:10.1126/sciadv.aao1054

Cited by 37 publications

(22 citation statements)

References 47 publications

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“…The detection of a 49 Ti excess in presolar SiC grains of SN origin, commonly referred to as X-grains, was interpreted by as evidence for the late formation of silicate carbide in type II SNe (Liu et al 2018). Detailed calculations show that 49 Ti must have been incorporated in the grains not sooner than 2 years after the explosion (Liu et al 2018), in agreement with theoretical calculations showing that SiC grains are late to form in the ejecta (Sarangi & Cherchneff 2015). Figure 2 shows that at that epoch more than 50% of the dust has already formed in the ejecta.…”

Section: The Growth Of Dust Mass In Sn Ejectamentioning

confidence: 99%

The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta

Dwek

Sarangi

Arendt

2019

ApJ

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Infrared (IR) observations of core collapse supernovae (CCSNe) have been used to infer the mass of dust that has formed in their ejecta. A plot of inferred dust masses versus supernova (SN) ages shows a trend of increasing dust mass with time, spanning a few decades of observations. This trend has been interpreted as evidence for the slow and gradual formation of dust in CCSNe. Observationally, the trend exhibits a t 2 behavior, exactly what is expected from an expanding optically thick ejecta. In this case, the observed dust resides in the infrared (IR)-thin "photosphere" of the ejecta, and constitutes only a fraction of the total dust mass. We therefore propose that dust formation proceeds very rapidly, condensing most available refractory elements within two years after the explosion. At early epochs, only a fraction of the dust emission escapes the ejecta accounting for the low observed dust mass. The ejecta's entire dust content is unveiled only a few decades after the explosion, with the gradual decrease in its IR opacity. Corroborating evidence for this picture includes the early depletions of refractory elements in the ejecta of SN1987A and the appearance of a silicate emission band around day 300 in SN 2004et.

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Section: The Growth Of Dust Mass In Sn Ejectamentioning

confidence: 99%

The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta

Dwek

Sarangi

Arendt

2019

ApJ

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“…For instance, supernova SiC grains are systematically 15 N rich and 54 Fe poor with respect to model predictions. Recent simulations suggest that many isotopic features of supernova SiC and graphite grains can be reproduced by H-ingestion in the Herich shells, that is, by the presence of residual H during explosive He-burning in supernova models (Pignatari et al 2013;Liu et al 2016Liu et al , 2017Liu et al , 2018. An alternative to selective mixing suggests the formation of supernova SiC and graphite grains in the O-rich layers of a massive star during a type II supernova explosion, where radiation may play a key role in dissociating the very stable CO molecules, hence freeing C atoms (Clayton et al 1999(Clayton et al , 2001Clayton 2013).…”

Section: Supernova Grainsmentioning

confidence: 99%

Binary Systems and Their Nuclear Explosions

Isern¹,

Hernanz²,

José³

2018

Astrophysics With Radioactive Isotopes

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“…However, several observational studies have presented evidence that dust formation must continue for years (Gall et al 2014, Wesson et al 2015, Bevan & Barlow 2016. Additional evidence for slow dust formation comes from studies of presolar dust grains in meteorites: Liu et al (2018) found that 49 Ti and 28 Si isotope ratios were consistent with dust forming after a significant fraction of 49 V (half-life 330 days) had decayed into 49 Ti, while Ott et al (2019) found that barium isotope ratios were consistent with silicon carbide dust grains having formed when a substantial fraction of 137 Cs (half-life 30 yr) had decayed into 137 Ba. Although the extraction of isotope ratios from presolar grains and the nucleosynthetic model adopted are both sources of significant uncertainty, these results also indicate that the bulk of the dust formation occurs years to decades after the supernova outburst.…”

Section: Introductionmentioning

confidence: 99%

Observational limits on the early-time dust mass in SN1987A

Wesson,

Bevan

2021

Preprint

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In recent years, dust masses of a few tenths of a solar mass have been found in the expanding ejecta of a number of core-collapse supernovae. How dust forms in such quantities remains poorly understood; theories of dust formation predict lower total masses and much faster formation rates than observations imply. One suggestion to reconcile observations and theory was made by Dwek et al. (2019), who proposed that the dust forms very rapidly, and because of its optical depth, is not initially observationally detectable, only being gradually revealed as the ejecta expand. Observational dust masses at early times would then only be lower limits. Using a large grid of radiative transfer models covering dust masses from 10 −4 to 1 M to calculate both the spectral energy distribution and the emission line profiles from clumpy dust shells, we show that this cannot be the case. Some clump distributions allow dust masses of ∼0.01 M to be concealed in clumps and still predict an SED consistent with the observations. However, these geometries predict emission line profiles which are inconsistent with the observations. Similarly, clump geometries which reproduce the observed emission line profiles with dust masses >0.01 M do not reproduce the SED. However, models with ∼10 −3 M of amorphous carbon can reproduce both the SED and the emission line profiles. We conclude that no large masses of dust can be hidden from view in the ejecta of SN 1987A at early epochs, and that the majority of dust must thus have formed at epochs >1000 days.

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Late formation of silicon carbide in type II supernovae

Abstract: Isotopic study of presolar grains shows supernova SiC dust condenses out of ejecta more than 2 years after the explosion.

Cited by 37 publications

References 47 publications

The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta

The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta

Binary Systems and Their Nuclear Explosions

Observational limits on the early-time dust mass in SN1987A

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