Dust and Molecular Formation in Supernovae

Matsuura, M.

doi:10.1007/978-3-319-20794-0_130-1

Cited by 4 publications

(7 citation statements)

References 180 publications

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“…9). Three of the no-dust detected SNe are of Type Ic and Ib/c SNe, which have fewer dust detections reported so far (Matsuura 2017). Other SNe are all Type II, mainly Type IIP, with one IIn and unclassified subclass (Table 1).…”

Section: Molecules As Precursor To Dust Formation?mentioning

confidence: 87%

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Dust in Supernovae and Supernova Remnants I: Formation Scenarios

2018

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Supernovae are considered as prime sources of dust in space. Observations of local supernovae over the past couple of decades have detected the presence of dust in supernova ejecta. The reddening of the high redshift quasars also indicate the presence of large masses of dust in early galaxies. Considering the top heavy IMF in the early galaxies, supernovae are assumed to be the major contributor to these large amounts of dust. However, the composition and morphology of dust grains formed in a supernova ejecta is yet to be understood with clarity. Moreover, the dust masses inferred from observations in mid-infrared and submillimeter wavelength regimes differ by two orders of magnitude or more. Therefore, the mechanism responsible for the synthesis of molecules and dust in such environments plays a crucial role in studying the evolution of cosmic dust in galaxies. This review summarises our current knowledge of dust formation in supernova ejecta and tries to quantify the role of supernovae as dust producers in a galaxy.

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Section: Molecules As Precursor To Dust Formation?mentioning

confidence: 87%

“…Next, we test the timing of molecule and dust formation/detections. We assumed the reported days of CO detections and ejecta dust detections from Matsuura (2017) and the histogram of these days are plotted in Fig. 10.…”

Section: Molecules As Precursor To Dust Formation?mentioning

confidence: 99%

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

2018

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“…Moreover, following the treatment of ISM dust by Guhathakurta & Draine (1989), it can be suggested that the smallest grains are much more prone to lose atoms from its surface at higher temperatures, which are analogous to the time of their genesis from the gas phase. Most importantly, the detection of molecules (Lepp et al 1990;Kotak et al 2009;Matsuura 2017) and atoms (Laming & Temim 2020) present in the gas also speaks against rapid growth of dust via accretion of all the residual gas-phase species on the surface of the grains.…”

Section: Discussionmentioning

confidence: 99%

“…The rapidly evolving ejecta of core-collapse supernovae (SNe) are known sites for the synthesis of cosmic dust (Bouchet & Danziger 1993;Wooden et al 1993;Dwek 2006;Szalai & Vinkó 2013;Matsuura 2017;Sarangi et al 2018b), and are often proposed to be the primary source of dust in high-redshift galaxies (Dwek et al 2007;Zhukovska et al 2008;Cherchneff & Dwek 2009;Gall et al 2011;Gall & Hjorth 2018). The mass and properties of dust present in SN ejecta are quantified by analyzing the spectral energy distribution (SED) at various wavelengths, where the mid-infrared (IR) and far-IR part of the SED is often dominated by emission from dust formed in the ejecta.…”

Section: Introductionmentioning

confidence: 99%

Formation, distribution, and IR emission of dust in the clumpy ejecta of Type II-P core-collapse supernovae, in isotropic and anisotropic scenarios

Sarangi

2022

A&A

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Large discrepancies are found between observational estimates and theoretical predictions when exploring the characteristics of dust formed in the ejecta of a core-collapse supernovae. We revisit the scenario of dust production in typical supernova ejecta in the first 3000 days after explosion, with an improved understanding of the evolving physical conditions and the distribution of the clumps. The generic, nonuniform distribution of dust within the ejecta was determined and using that, the relevant opacities and fluxes were calculated. The dependence of the emerging fluxes on the viewing angle was estimated for an anisotropic, ellipsoidal geometry of the ejecta that imitate SN 1987A. We model the He core from the center to its outer edge as 450 stratified, clumpy, annular shells, uniquely identified by their distinct velocities and characterized by their variations in abundances, densities, and gas and dust temperatures. We find that the formation of dust starts between day 450 and day 550 post-explosion, and it continues until about day 2800, although the first 1600 days are the most productive. The total dust mass evolves from ∼ 10 −5 M at day 500 to 10 −3 M at day 800, finally saturating at about 0.06 M . The masses of the O-rich dust (silicates, alumina) dominates the C-rich dust (amorphous carbon, silicon carbide) at all times; the formation of carbon dust is delayed beyond 2000 days post-explosion. We show that the opacities are largest between days 800 and 1600, and the characteristic spectral features of O-rich dust species are suppressed at those times. The fluxes emerging along the smallest axes of the ellipsoidal ejecta are found to be the most obscured, while a viewing angle between 16 to 21 • with that axis appears to be in best agreement with the fluxes from SN 1987A at days 615 and 775.

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“…SN1987A was the first SN in which dust formation was reported (Danziger et al 1989). Since then dust formation has been reported in over ten SNe and a few SNRs (Gall et al 2014;Matsuura 2017; with the inferred dust masses in young SNe typically of the order of 10 −6 to 10 −3 M (e.g. Wooden et al 1993;Bouchet et al 2004;Kotak et al 2009).…”

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confidence: 99%

SOFIA mid-infrared observations of Supernova 1987A in 2016 – forward shocks and possible dust re-formation in the post-shocked region

Matsuura

Buizer

Arendt

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The equatorial ring of Supernova (SN) 1987A has been exposed to forward shocks from the SN blast wave, and it has been suggested that these forward shocks have been causing on-going destruction of dust in the ring. We obtained SOFIA FORCAST 11.1, 19.7 and 31.5 µm photometry of SN 1987A in 2016. Compared with Spitzer measurements 10 years earlier, the 31.5 µm flux has significantly increased. The excess at 31.5 µm appears to be related to the Herschel 70 µm excess, which was detected 5 years earlier. The dust mass needed to account for the the 31.5-70 µm excess is 3-7×10 −4 M , more than ten times larger than the ring dust mass (∼ 1 × 10 −5 M ) estimate from the data 10-years earlier. We argue that dust grains are re-formed or grown in the post-shock regions in the ring after forward shocks have destroyed pre-existing dust grains in the ring and released refractory elements into gas. In the post-shock region, atoms can stick to surviving dust grains, and the dust mass may have increased (grain growth), or dust grains might have condensed directly from the gas. An alternative possibility is that the outer part of the expanding ejecta dust might have been heated by X-ray emission from the circumstellar ring. The future development of this excess could reveal whether grains are reformed in the post-shocked region of the ring or eject dust is heated by X-ray.

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Dust and Molecular Formation in Supernovae

Cited by 4 publications

References 180 publications

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

Formation, distribution, and IR emission of dust in the clumpy ejecta of Type II-P core-collapse supernovae, in isotropic and anisotropic scenarios

SOFIA mid-infrared observations of Supernova 1987A in 2016 – forward shocks and possible dust re-formation in the post-shocked region

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