Type Ib/Ic Supernovae: Effect of Nickel Mixing on the Early-time Color Evolution and Implications for the Progenitors

Yoon, Sung Chul; Chun, Wonseok; Tolstov, Alexey; Блинников, С. И.

doi:10.3847/1538-4357/ab0020

Cited by 40 publications

(79 citation statements)

References 105 publications

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“…They do show that as the mixing of 56 Ni increases, the rise time increases, which matches our work. The B-V values in Yoon et al (2019) show that the least mixed models have a lower B-V at peak and the fully have the highest B-V at peak if we only consider the time range of only -2 to 12 days from peak, similar to the time range in our work. This matches our results in Figure 10.…”

Section: Discussionsupporting

confidence: 70%

“…Section 5 shows that both fully and partially mixed models can replicate features much better across multiple epochs for various observed SNe. Yoon et al (2019) discusses the affect of 56 Ni mixing in the very early phases of the explosion. Their code and work considers phases with respect to peak of -10 to -25 days and include the contribution of breakout emission.…”

Section: Discussionmentioning

confidence: 99%

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Type Ic supernova of a 22 M⊙ progenitor

Teffs

Ertl

Mazzali

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Type Ic supernovae (SNe Ic) are a sub-class of core-collapse supernovae that exhibit no helium or hydrogen lines in their spectra. Their progenitors are thought to be bare carbon-oxygen cores formed during the evolution of massive stars that are stripped of their hydrogen and helium envelopes sometime before collapse. SNe Ic present a range of luminosities and spectral properties, from luminous GRB-SNe with broad-lined spectra to less luminous events with narrow-line spectra. Modelling SNe Ic reveals a wide range of both kinetic energies, ejecta masses, and 56 Ni masses. To explore this diversity and how it comes about, light curves and spectra are computed from the ejecta following the explosion of an initially 22 M ⊙ progenitor that was artificially stripped of its hydrogen and helium shells, producing a bare CO core of ∼ 5 M ⊙ , resulting in an ejected mass of ∼ 4 M ⊙ , which is an average value for SNe Ic. Four different explosion energies are used that cover a range of observed SNe. Finally, 56 Ni and other elements are artificially mixed in the ejecta using two approximations to determine how element distribution affects light curves and spectra. The combination of different explosion energy and degree of mixing produces spectra that roughly replicate the distribution of near-peak spectroscopic features of SNe Ic. High explosion energies combined with extensive mixing can produce red, broad-lined spectra, while minimal mixing and a lower explosion energy produce bluer, narrow-lined spectra.

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Section: Discussionsupporting

confidence: 70%

Section: Discussionmentioning

confidence: 99%

Type Ic supernova of a 22 M⊙ progenitor

Teffs

Ertl

Mazzali

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…A relatively low degree of 56 Ni mixing is also suggested by the comparison of the early colors of LSQ13abf to the models developed by Yoon et al (2019). We show this comparison in Fig.…”

Section: Hydrodynamical Models With a Double 56 Ni Distributionsupporting

confidence: 66%

“…14, where low degree of 56 Ni mixing ( f m ) produce models with double-peaked color curves, while strong 56 Ni mixing produces monotonically-rising color curves. LSQ13abf shows a double peak in the color curves, and a slow rise to the second main peak, like other SNe Ib in the literature, and in contrast to most SNe Ic, as shown by Yoon et al (2019) in their Fig. 11.…”

Section: Hydrodynamical Models With a Double 56 Ni Distributionsupporting

confidence: 57%

The Carnegie Supernova Project II

Stritzinger¹,

Taddia²,

Holmbo³

et al. 2020

A&A

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Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M⊙, a 56Ni mass of 0.16 ± 0.02 M⊙, and a progenitor-star radius of 28.0 ± 7.5 R⊙. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M⊙ zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of ≳20−25 M⊙ zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of ≲10 M⊙ and extended (∼100 R⊙) envelopes also broadly match the observations of LSQ13abf.

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“…The short rise times and large peak luminosities of SNe Ibc suggest that weak mixing is unlikely in SNe Ibc. Simulations for varying levels of mixing have been presented earlier (Dessart et al 2012(Dessart et al , 2015; see also Yoon et al 2019).…”

Section: Radiation-hydrodynamics Simulations Of the Explosion With V1dmentioning

confidence: 99%

Supernovae Ib and Ic from the explosion of helium stars

Dessart

Yoon

Aguilera-Dena

et al. 2020

A&A

Self Cite

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Much difficulty has so far prevented the emergence of a consistent scenario for the origin of Type Ib and Ic supernovae (SNe). Either the SN rates or the ejecta masses and composition were in tension with inferred properties from observations. Here, we follow a heuristic approach by examining the fate of helium stars in the mass range from 4 to 12 M⊙, which presumably form in interacting binaries. The helium stars were evolved using stellar wind mass loss rates that agree with observations and which reproduce the observed luminosity range of galactic Wolf-Rayet stars, leading to stellar masses at core collapse in the range from 3 to 5.5 M⊙. We then exploded these models adopting an explosion energy proportional to the ejecta mass, which is roughly consistent with theoretical predictions. We imposed a fixed 56Ni mass and strong mixing. The SN radiation from 3 to 100 d was computed self-consistently, starting from the input stellar models using the time-dependent nonlocal thermodynamic equilibrium radiative-transfer code CMFGEN. By design, our fiducial models yield very similar light curves, with a rise time of about 20 d and a peak luminosity of ~1042.2 erg s−1, which is in line with representative SNe Ibc. The less massive progenitors retain a He-rich envelope and reproduce the color, line widths, and line strengths of a representative sample of SNe Ib, while stellar winds remove most of the helium in the more massive progenitors, whose spectra match typical SNe Ic in detail. The transition between the predicted Ib-like and Ic-like spectra is continuous, but it is sharp, such that the resulting models essentially form a dichotomy. Further models computed with varying explosion energy, 56Ni mass, and long-term power injection from the remnant show that a moderate variation of these parameters can reproduce much of the diversity of SNe Ibc. We conclude that massive stars stripped by a binary companion can account for the vast majority of ordinary Type Ib and Ic SNe and that stellar wind mass loss is the key to removing the helium envelope in the progenitors of SNe Ic.

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Type Ib/Ic Supernovae: Effect of Nickel Mixing on the Early-time Color Evolution and Implications for the Progenitors

Cited by 40 publications

References 105 publications

Type Ic supernova of a 22 M⊙ progenitor

Type Ic supernova of a 22 M⊙ progenitor

The Carnegie Supernova Project II

Supernovae Ib and Ic from the explosion of helium stars

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