Airborne spectrophotometry of SN 1987A from 1.7 to 12.6 microns - Time history of the dust continuum and line emission

Wooden, D. H.; Rank, D. M.; Bregman, J. D.; Witteborn, F. C.; Tielens, A. G. G. M.; Cohen, Martin; Pinto, Philip A.; Axelrod, T. S.

doi:10.1086/191830

Cited by 212 publications

(245 citation statements)

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“…The analysis is insensitive to temperature due to the low excitation potential (0.18 eV) for the first excited state giving the [Ni II] 6.636 µm line. Wooden et al (1993) extended the analysis to later times, finding a similar value. In the ejecta models of J12/J14, LTE is valid for the [Ni II] 6.636 µm line throughout this period.…”

Section: Discussion and Summarymentioning

confidence: 64%

“…Regarding ionization, we find about 80% of the nickel being singly ionized between 250 and 450 days, with most of the remainder being Ni III. The most questionable assumption in the Rank et al (1988) and Wooden et al (1993) derivation is that of optically thin emission; in our models the [Ni II] 6.636 µm line has an optical depth of 3.2 at 250 days and 1.5 at 450 days. This optical depth leads to an underestimate of the Ni mass by a factor of 2-3 if one uses the optically thin formula.…”

Section: Discussion and Summarymentioning

confidence: 97%

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Supersolar Ni/Fe production in the Type IIP SN 2012ec

Jerkstrand

Smartt

Sollerman

et al. 2015

Monthly Notices of the Royal Astronomical Society

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SN 2012ec is a Type IIP supernova (SN) with a progenitor detection and comprehensive photospheric-phase observational coverage. Here, we present Very Large Telescope and PESSTO observations of this SN in the nebular phase. We model the nebular [O I] λλ6300, 6364 lines and find their strength to suggest a progenitor main-sequence mass of 13 − 15 M ⊙ . SN 2012ec is unique among hydrogen-rich SNe in showing a distinct line of stable nickel [Ni II] λ7378. This line is produced by 58 Ni, a nuclear burning ash whose abundance is a sensitive tracer of explosive burning conditions. Using spectral synthesis modelling, we use the relative strengths of [Ni II] λ7378 and [Fe II] λ7155 (the progenitor of which is 56 Ni) to derive a Ni/Fe production ratio of 0.20 ± 0.07 (by mass), which is a factor 3.4 ± 1.2 times the solar value. High production of stable nickel is confirmed by a strong [Ni II] 1.939 µm line. This is the third reported case of a core-collapse supernova producing a Ni/Fe ratio far above the solar value, which has implications for core-collapse explosion theory and galactic chemical evolution models.

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Section: Discussion and Summarymentioning

confidence: 64%

Section: Discussion and Summarymentioning

confidence: 97%

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Jerkstrand

Smartt

Sollerman

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…In analogy to the well-studied type IIb SN 1993J, some 0.6 M of condensible elements (C, Mg, Si, S & Fe) were ejected during the SN explosion of Cas A (Thielemann et al 1996), corresponding to a very high dust formation efficiency of ∼ 0.2. Likewise, Herschel observations of the extremely young SNR associated with SN 1987A -which has just entered the reverse shock phase as the ejecta slammed into the previous stellar wind remnant some 10 years after the explosion -reveal ∼ 0.5 M of cold dust † (Matsuura et al 2011); many orders of magnitude larger than estimated from observations during the dust condensation period of ∼ 500 − 1000 days (Wooden et al 1993). Given the bewildering zoo of SNe types and the uncertainties and conflicting observational results on dust formation in these environments, the contribution of SNe to the dust budget can presently only be guessed at but this anecdotal evidence suggests that it is high.…”

Section: Sources Of Stardustmentioning

confidence: 96%

“…Observationally, dust is known to form typically between 300 and 1000 days after the SN explosion as revealed by a sudden drop in optical light, a concommittant increase in IR emission, and the development of a pronounced bluered asymmetry in the emission line profiles of the ejecta (Wooden et al 1993, Lucy et al 1989. However, IR studies of core collapse SNe implied less than 5 × 10 −3 M of dust (somewhat dependent on the adopted grain material properties, very sensitive to the adopted clumpy distribution of the ejecta, and widely varying between SNe), corresponding to an efficiency of 10 −3 − 10 −1 (Wooden et al 1993, Sugarman et al 2006, Ercolano et al 2007, Meikle et al 2007see Barlow 2009 for a recent review). Young supernova remnants (SNR) provide another view of the dust formation efficiency of SNe and one that indicates much higher dust formation efficiencies.…”

Section: Sources Of Stardustmentioning

confidence: 99%

Chemical and physical properties of interstellar dust

Tielens¹

2011

Proc. IAU

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Abstract. The characteristics of interstellar dust reflect a complex interplay between stellar injection of stardust, destruction in the ISM, and regrowth in clouds. Astronomical observations and analysis of stardust isolated from meteorites have revealed a highly diverse interstellar and circumstellar grain inventory, including both amorphous materials and highly crystalline compounds (silicates and carbon). This review summarizes this dust budget and inventory. Interstellar dust is highly processed during its sojourn from its birthsite (stellar ejecta) to its incorporation into protoplanetary systems. Processing by strong shocks due to supernova explosions is particularly important. Sputtering by impacting gas ions in shocks in the intercloud medium of the ISM is counteracted by accretion in cloud phases and their balance sets the observed, interstellar, elemental depletion patterns. Astronomical and meteoritical-stardust evidence for these processes is reviewed and it is concluded that dust formation in the ISM is very rapid. Not surprisingly, the characteristics of interstellar dust are expected to vary widely reflecting local stellar sources, the effects of SNe processing, and the interstellar accretion process.

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“…SN 1987A was the first core-collapse supernova with evidence for dust formation two years after the explosion. The reported dust masses in those early days were 10 −6 to 10 −5 M (Bouchet et al 1991;Wooden et al 1993).…”

Section: Introductionmentioning

confidence: 99%

Measuring the dust content and formation in SN 1987A using detailed radiative transfer modelling

et al. 2017

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Abstract. Core-collapse supernovae are expected to be efficient producers of dust, and recent Herschel and ALMA observations have revealed up to 1 M of cold dust in the inner ejecta of SN 1987A. The formation time scale, spatial distribution and clumpiness, and the importance of the different heating sources of the dust remain poorly understood. We have started a project to make detailed 3D dust radiative transfer models for SN 1987A, based on a combination of the latest observational constraints and input from 3D hydrodynamical models and dust formation models. Preliminary results seem to indicate the need for large, micron-sized dust grains, and a relatively large dust mass.

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Airborne spectrophotometry of SN 1987A from 1.7 to 12.6 microns - Time history of the dust continuum and line emission

Cited by 212 publications

References 0 publications

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Chemical and physical properties of interstellar dust

Measuring the dust content and formation in SN 1987A using detailed radiative transfer modelling

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