The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination

Mazzali, P. A.; Bikmaev, I.; Sunyaev, R.; Ashall, C.; Prentice, S.; Tanaka, Masaomi; Irtuganov, E.; Melnikov, S. S.; Zhuchkov, R. Ya.

doi:10.1093/mnras/staa839

Cited by 23 publications

(21 citation statements)

References 63 publications

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“…The fraction of the bolometric luminosity emitted in the MIR fine-structure lines remains unclear. Recent observational (e.g., Black et al 2016, Mazzali et al 2020 Fine-structure cooling will occur only in the low-density regions in a clumpy medium. Due to these uncertainties, we include the fraction of total luminosity emitted in the optical and NIR as a free parameter in our subsequent analyses.…”

Section: Constructing the Pseudo-bolometric Light Curvementioning

confidence: 99%

The Whisper of a Whimper of a Bang: 2400 Days of the Type Ia SN 2011fe Reveals the Decay of $^{55}$Fe

Tucker¹,

Shappee²,

Kochanek³

et al. 2021

Preprint

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We analyze new multi-filter Hubble Space Telescope (HST) photometry of the normal Type Ia supernova (SN Ia) 2011fe out to ≈ 2400 days after maximum light, the latest observations to-date of a SN Ia. We model the pseudo-bolometric light curve with a simple radioactive decay model and find energy input from both 57 Co and 55 Fe are needed to power the late-time luminosity. This is the first detection of 55 Fe in a SN Ia. We consider potential sources of contamination such as a surviving companion star or delaying the deposition timescale for 56 Co positrons but these scenarios are ultimately disfavored. The relative isotopic abundances place direct constraints on the burning conditions experienced by the white dwarf and require a central density of ρ c ∼ 3 × 10 8 g cm −3 . Only 2 classes of explosion models are currently consistent with all observations of SN 2011fe: 1) the delayed detonation of a low-ρ c , near-M Ch (1.2 − 1.3M ) WD, or 2) a sub-M Ch (1.0 − 1.1 M ) WD experiencing a thin-shell double detonation.

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Section: Constructing the Pseudo-bolometric Light Curvementioning

confidence: 99%

The Whisper of a Whimper of a Bang: 2400 Days of the Type Ia SN 2011fe Reveals the Decay of $^{55}$Fe

Tucker¹,

Shappee²,

Kochanek³

et al. 2021

Preprint

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show abstract

“…Lacking a definitive bolometric light curve 1 we cannot confidently estimate the overall 56 Ni mass, which affects the excitation of the central oxygen at late times. The lack of a nebular spectral series makes it difficult to determine accurately the densities in the inner layers: the changing ionization as a function of time is very important in this respect (e.g., Mazzali & Hachinger 2012;Mazzali et al 2020).…”

Section: Discussionmentioning

confidence: 99%

A very low central oxygen mass in the peculiar type Ia SN 2010lp: further diversity at the low-luminosity end of SNe Ia

Mazzali,

Benetti,

Stritzinger

et al. 2022

Preprint

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A nebular spectrum of the peculiar, low-luminosity type Ia supernova 2010lp is modelled in order to estimate the composition of the inner ejecta and to illuminate the nature of this event. Despite having a normally declining light curve, SN 2010lp was similar spectroscopically to SN 1991bg at early times. However, it showed a very unusual double-peaked [O I] λλ 6300, 6363 emission at late times (Taubenberger et al. 2013). Modelling of the nebular spectrum suggests that a very small amount of oxygen (∼ 0.05 M ⊙ ), expanding at very low speed ( ∼ < 2000 km s −1 ) is sufficient to reproduce the observed emission. The rest of the nebula is not too dissimilar from SN 1991bg, except that SN 2010lp is slightly more luminous. The double-peaked [O I] emission suggests that SN 2010lp may be consistent with the merger or collision of two low-mass white dwarfs. The low end of the SN Ia luminosity sequence is clearly populated by diverse events, where different channels may contribute.

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“…We propose that clumping may explain this discrepancy. Clumping in the ejecta of SNe Ia has been suggested by both observational (e.g., Black et al 2016;Mazzali et al 2020) and theoretical (e.g., Wilk et al 2020) studies but confirmation is difficult. Clumping determines where energy deposition occurs as clumps will retain energy input from radioactive decays more efficiently than the lower-density regions between them.…”

Section: Discussionmentioning

confidence: 99%

A Rapid Ionization Change in the Nebular-Phase Spectra of the Type Ia SN 2011fe

Tucker,

Ashall,

Shappee

et al. 2021

Preprint

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We present three new spectra of the nearby Type Ia supernova (SN Ia) 2011fe covering ≈ 480 − 850 days after maximum light and show that the ejecta undergoes a rapid ionization shift at ∼ 500 days after explosion. The prominent [Fe III] emission lines at ≈ 4600 Å are replaced with the permitted Fe I+Fe II blends at ∼ 4400 Å and ∼ 5400 Å. The ≈ 7300 Å feature, which is produced by [Fe II] +[Ni II] at 400 days after explosion, is replaced by broad (≈ ±15 000 km s −1 ) symmetric [Ca II] emission. The change in emission characteristics is likely due to the temperature in the inner ejecta dropping below the level needed to populate the high-ionization Fe III transitions. This ionization shift corresponds to a distinct temperature and density in the ejecta and may be useful as a probe of the ejecta's temporal evolution. Models predict this ionization transition occurring ∼ 100 days later than what is observed which we attribute to clumping in the ejecta. Finally, we discuss the reliability of [Ca II] as an ejecta diagnostic feature.

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The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination

Cited by 23 publications

References 63 publications

The Whisper of a Whimper of a Bang: 2400 Days of the Type Ia SN 2011fe Reveals the Decay of $^{55}$Fe

The Whisper of a Whimper of a Bang: 2400 Days of the Type Ia SN 2011fe Reveals the Decay of $^{55}$Fe

A very low central oxygen mass in the peculiar type Ia SN 2010lp: further diversity at the low-luminosity end of SNe Ia

A Rapid Ionization Change in the Nebular-Phase Spectra of the Type Ia SN 2011fe

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