Type IIn SN 2010jl: probing dusty line-emitting shell

Чугай, Н. Н.

doi:10.1093/mnras/sty2386

Cited by 30 publications

(31 citation statements)

References 45 publications

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“…The BWC has been frequently attributed to the effects of electron scattering in SN 2010jl, and this is certainly an important effect at early times (Fransson et al 2014). At later times, however, the asymmetric, non-Lorentzian shape suggests a alternative origin for the BWC (Gall et al 2014;Chugai 2018). We therefore attribute the BWC to fast-moving ejecta.…”

Section: Model Geometrymentioning

confidence: 81%

“…The persistence of asymmetrical lines to very late times (>1000 days) when the photosphere has entirely receded rules out line optical depth effects at late times (Chugai 2018), and, while scattering by electrons in the CSM could cause longlasting line shifting, it would affect all lines similarly and would not account for the asymmetrical line shapes that are observed. Finally, the simultaneous presence of a significant IR excess combined with the wavelength dependence of the line blueshifting, as discussed by Gall et al (2014) and Smith et al (2012), strongly favors a dust formation scenario, with dust grains condensing in a CDS between the shock fronts or in the ejecta itself.…”

Section: Asymmetric Emission-line Profilesmentioning

confidence: 99%

“…The IR excess can also be caused by preexisting circumstellar dust heated by the UV flash, but preexisting dust likely only makes a significant contribution to the IR excess at early times because it fades rapidly for most geometries. SN 2010jl exhibited an IR excess at early and later stages along with blueshifted line profiles, leading a number of authors to infer the formation of new dust in its CDS and/or in its ejecta (e.g., Andrews et al 2011;Smith et al 2012;Maeda et al 2013;Fransson et al 2014;Gall et al 2014;Chugai 2018;Sarangi et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Disentangling Dust Components in SN 2010jl: The First 1400 Days

Bevan

Krafton

Wesson

et al. 2020

ApJ

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The luminous Type IIn SN 2010jl shows strong signs of interaction between the SN ejecta and dense circumstellar material. Dust may be present in the unshocked ejecta; the cool, dense shell (CDS) between the shocks in the interaction region; or in the circumstellar medium (CSM). We present and model new optical and infrared photometry and spectroscopy of SN 2010jl from 82 to 1367 days since explosion. We evaluate the photometric and spectroscopic evolution using the radiative transfer codes MOCASSIN and DAMOCLES, respectively. We propose an interaction scenario and investigate the resulting dust formation scenarios and dust masses. We find that SN 2010jl has been continuously forming dust based on the evolution of its infrared emission and optical spectra. There is evidence for preexisting dust in the CSM as well as new dust formation in the CDS and/or ejecta. We estimate that 0.005-0.01 M e of predominantly carbon dust grains has formed in SN 2010jl by ∼1400 days post-outburst. Unified Astronomy Thesaurus concepts: Core-collapse supernovae (304); Type II supernovae (1731); Circumstellar dust (236); Dust continuum emission (412); Dust nebulae (413); Astronomical models (86); Radiative transfer (1335); Extinction (505); Circumstellar shells (242); Dust shells (414)

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Section: Model Geometrymentioning

confidence: 81%

Section: Asymmetric Emission-line Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Disentangling Dust Components in SN 2010jl: The First 1400 Days

Bevan

Krafton

Wesson

et al. 2020

ApJ

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“…Several studies of type IIn SNe (which, in some cases, may have an LBV as progenitor) are a good example (e.g. Smith et al 2008b;Fox et al 2009;Gall et al 2014;Andrews et al 2016;Chugai 2018). Grain growth may also be a viable mechanism as explained by Kirchschlager et al (2020).…”

Section: Potential Dust Survival From Sn Explosionsmentioning

confidence: 99%

The contribution by luminous blue variable stars to the dust content of the Magellanic Clouds

Agliozzo

Phillips

Mehner

et al. 2021

A&A

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Context. Previous studies have concluded that low- and intermediate-mass stars cannot account for the interstellar dust yield in the Magellanic Clouds inferred from far-infrared and sub-millimetre observations. Aims. Luminous blue variable stars (LBVs) form dust as a result of episodic, violent mass loss. To investigate their contribution as dust producers in the Magellanic Clouds, we analyse 31 confirmed and candidate LBVs from a recent census. Methods. We built a maximally complete multi-wavelength dataset of these sources from archival space telescope images and catalogues from near-infrared to millimetre wavelengths. We also present new Very Large Telescope VISIR observations of three sources in the Large Magellanic Cloud (LMC). We review the LBV classification on the basis of the infrared spectral energy distribution. To derive characteristic dust parameters, we fitted the photometry resulting from a stacking analysis, which consists of co-adding images of the same wavelength band of several targets to improve the signal-to-noise. For comparison we also stacked the images of low- and intermediate-mass evolved stars in the LMC. Results. We find four classes of sources: (1) LBVs showing mid-infrared dust emission plus near-infrared free-free emission from an ionised stellar wind (Class 1a) or only mid-infrared dust emission (Class 1b); (2) LBVs with a near-infrared excess due to free-free emission only (Class 2); (3) objects with an sgB[e] classification in the literature, displaying a distinctive hot dust component; and (4) objects with no detected stellar winds and no circumstellar matter in their SEDs. From the stacking analysis of the 18 Class 1 and 2 objects in the LMC, we derived an integrated dust mass of 0.11−0.03+0.06 M⊙. This is two orders of magnitude larger than the value inferred from stacking 1342 extreme-asymptotic giant branch stars. The dust mass of individual LBVs does not correlate with the stellar parameters, possibly suggesting that the dust production mechanism is independent of the initial stellar mass or that the stars have different evolutionary histories. The total dust yield from LBVs over the age of the LMC is ∼104 − 105 M⊙. The one order of magnitude uncertainty is mainly due to uncertainties of the LBV population, star formation history, and initial mass function. Conclusions. LBVs are potentially the second most important source of dust in normal galaxies. The role of dust destruction in LBV nebulae by a possible subsequent supernova (SN) blast wave has yet to be determined. Recent theoretical developments in the field of dust processing by SN shocks highlight the potential survival of dust grains from the pre-existing circumstellar nebula.

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“…Some researches interpret the IR excess as the evidence of newly-formed dust (Smith et al 2012;Maeda et al 2013;Gall et al 2014), while others suggest a pre-existing and unshocked CSM dust grains (Andrews et al 2011;Fox et al 2013;Fransson et al 2014). Moreover, Bevan et al (2020) and Chugai (2018) propose that SN 2010jl presents both evidence of pre-existing dust in CSM and newly-formed dust in cold dense shell and/or ejecta. Gall et al (2014) derived the extinction curves of SN 2010jl from the attenuation of emission lines, and found rapid (in 40 -240 days) dust formation and inferred the presence of very large (> 1 micron) grains.…”

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confidence: 99%

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

Li,

Gao,

Jiang

et al. 2022

Preprint

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The unusual extinction curves of SN 2010jl provide an excellent opportunity to investigate the properties of dust formed by core-collapse supernovae. By using a series of dust models with different compositions and grain size distributions, we fit the extinction curves of SN 2010jl and find that a silicate-graphite mixture dust model characterized by exponentially cutoff powerlaw size distributions can well reproduce its unusual extinction curves. The best-fit results show that the extinctions derived from the dust models are consistent with the observed values at all epochs. However, the total-to-selective extinction ratio 𝑅 𝑉 is about 2.8 -3.1, which is significantly smaller than the value of 𝑅 𝑉 ≈ 6.4 derived by Gall et al. The best-fit models indicate that the dust grains around SN 2010jl are possibly composed of small-size astronomical silicate grains and micron-size graphite grains. In addition, by fitting the optical to mid-infrared spectral energy distribution, we find that the dust mass around SN 2010jl increases with time, up to 0.005 𝑀 around 1300 days after peak brightness, which is consistent with previous estimates.

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Type IIn SN 2010jl: probing dusty line-emitting shell

Cited by 30 publications

References 45 publications

Disentangling Dust Components in SN 2010jl: The First 1400 Days

Disentangling Dust Components in SN 2010jl: The First 1400 Days

The contribution by luminous blue variable stars to the dust content of the Magellanic Clouds

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

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