DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

Kotak, R.; Meikle, W. P. S.; Farrah, D.; Gerardy, C.; Foley, R. J.; Dyk, Schuyler D. Van; Fransson, Claes; Lundqvist, Peter; Sollerman, J.; Fesen, Robert A.; Filippenko, A. V.; Mattila, S.; Silverman, J. M.; Andersen, Anja C.; Höflich, Peter; Pozzo, Monica; Wheeler, J. C.

doi:10.1088/0004-637x/704/1/306

Cited by 187 publications

(339 citation statements)

References 82 publications

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“…Taking the optical depth into account, the Ni/Fe ratio in SN 1987A is around solar or somewhat higher. Jerkstrand et al (2012) calculated the model luminosity of [Ni II] 6.636 µm at 350d using the Woosley & Heger (2007) nucleosynthesis models, finding good agreement with the observed line in SN 2004et (Kotak et al 2009). As mentioned above, however, a caveat is that the nickel line has an optical depth of a few at these epochs, so the model luminosity depends not only on the nickel mass but also on the volume of the nickel-containing gas.…”

Section: Discussion and Summarymentioning

confidence: 58%

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: 58%

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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“…Two types of dust are assumed, either carbon or silicates, or a mixture of both, and dust masses are derived (e.g., Sugerman et al 2006;Ercolano et al 2007;Kotak et al 2009). As our results illustrate, the final size distributions obtained for dust grains that condense in homogenous and clumpy ejecta do not follow such a power-law distribution.…”

Section: Summary and Discussionmentioning

confidence: 99%

Condensation of dust in the ejecta of Type II-P supernovae

Sarangi

Cherchneff

2015

A&A

138

189

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Aims. We study the production of dust in Type II-P supernova ejecta by coupling the gas-phase chemistry to the dust nucleation and condensation phases. We consider two supernova progenitor masses with homogeneous and clumpy ejecta to assess the chemical type and quantity of dust that forms. Grain size distributions are derived for all dust components as a function of post-explosion time.Methods. The chemistry of the gas phase and the simultaneous formation of dust clusters are described by a chemical network that includes all possible processes that are efficient at high gas temperatures and densities. The formation of key bimolecular species (e.g., CO, SiO) and dust clusters of silicates, alumina, silica, metal carbides, metal sulphides, pure metals, and amorphous carbon is considered. A set of stiff, coupled, ordinary, differential equations is solved for the gas conditions pertaining to supernova explosions. These master equations are coupled to a dust condensation formalism based on Brownian coagulation. Results. We find that Type II-P supernovae produce dust grains of various chemical compositions and size distributions as a function of post-explosion time. The grain size distributions gain in complexity with time, are slewed towards large grains, and differ from the usual Mathis, Rumpl, & Nordsieck power-law distribution characterising interstellar dust. Gas density enhancements in the form of ejecta clumps strongly affect the chemical composition of dust and the grain size distributions. Some dust type, such as forsterite and pure metallic grains, are highly dependent on clumpiness. Specifically, a clumpy ejecta produces large grains over 0.1 µm, and the final dust mass for the 19 M progenitor reaches 0.14 M . Clumps also favour the formation of specific molecules, such as CO 2 , in the oxygen-rich zones. Conversely, the carbon and alumina dust masses are primarily controlled by the mass yields of alumina and carbon in the ejecta zones where the dust is produced. The supernova progenitor mass and the 56 Ni mass also affect dust production. Our results highlight that dust synthesis in Type II-P supernovae is not a single and simple process, as often assumed. Several dust components form in the ejecta over time and the total dust mass gradually builds up over a time span around three to five years post-outburst. This gradual growth provides a possible explanation for the discrepancy between the small amounts of dust formed at early post-explosion times and the high dust masses derived from recent observations of supernova remnants.

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“…Dwek et al (2007) propose 1 M of dust per SN will be necessary to account for dust masses in high-z QSOs, while contemplating SNe as the only source. Such high dust masses for SNe contradict derived dust masses from nearby SNe and SN remnants, which on average reveal a few times 10 −4 -10 −2 M of dust (e.g., Wooden et al 1993;Elmhamdi et al 2003;Temim et al 2006;Meikle et al 2007;Rho et al 2008;Kotak et al 2009;Sibthorpe et al 2010;Barlow et al 2010). A review of observationally and theoretically derived dust from stellar sources is provided by Gall et al (in prep.,herafter GAH11).…”

Section: Introductionmentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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Aims. The aim is to elucidate the astrophysical conditions required for generating large amounts of dust in massive starburst galaxies at high redshift. Methods. We have developed a numerical galactic chemical evolution model. The model is constructed such that the effect of a wide range of parameters can be investigated. It takes into account results from stellar evolution models, a differentiation between diverse types of core collapse supernovae (CCSN), and the contribution of asymptotic giant branch (AGB) stars in the mass range 3-8 M . We consider the lifetime-dependent yield injection into the interstellar medium (ISM) by all sources, and dust destruction due to supernova (SN) shocks in the ISM. We ascertain the temporal progression of the dust mass and the dust-to-gas and dust-to-metal mass ratios, as well as other physical properties of a galaxy, and study their dependence on the mass of the galaxy, the initial mass function (IMF), dust production efficiencies, and dust destruction in the ISM. Results. The amount of dust and the physical properties of a galaxy strongly depend on the initial gas mass available. Overall, while the total amount of dust produced increases with galaxy mass, the detailed outcome depends on the SN dust production efficiency, the IMF, and the strength of dust destruction in the ISM. Dust masses are higher for IMFs biased towards higher stellar masses, even though these IMFs are more strongly affected by dust destruction in the ISM. The sensitivity to the IMF increases as the mass of the galaxy decreases. SNe are primarily responsible for a significant enrichment with dust at early epochs (<200 Myr). Dust production with a dominant contribution by AGB stars is found to be insufficient to account for dust masses in excess of 10 8 M within 400 Myr after starburst. Conclusions. We find that galaxies with initial gas masses between 1-5 × 10 11 M are massive enough to enable production of dust masses >10 8 M . Our preferred scenario is dominated by SN dust production in combination with top-heavy IMFs and moderate dust destruction in the ISM.

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DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

Cited by 187 publications

References 82 publications

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

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

Condensation of dust in the ejecta of Type II-P supernovae

Genesis and evolution of dust in galaxies in the early Universe

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