Supernovae Ib and Ic from the explosion of helium stars

Dessart, Luc; Yoon, Sung‐Chul; Aguilera-Dena, David R.; Langer, N.

doi:10.1051/0004-6361/202038763

Cited by 54 publications

(76 citation statements)

References 120 publications

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“…The final masses of our models with Z = 0.02 are in agreement with Yoon (2017) and Dessart et al (2020). The final masses and lifetimes of our Z = 0.015 models are also consistent with the Z = 0.0145 models from Woosley (2019) at masses where the WC/WO wind is unimportant.…”

Section: Comparison To Previous Stellar Evolution Modelssupporting

confidence: 80%

Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Aguilera-Dena,

Langer,

Antoniadis

et al. 2021

Preprint

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Massive stars that become stripped of their hydrogen envelope through binary interaction or winds can be observed either as Wolf-Rayet stars, if they have optically thick winds, or as transparent-wind stripped-envelope stars. We approximate their evolution through evolutionary models of single helium stars, and compute detailed model grids in the initial mass range 1.5 to 70 M for metallicities between 0.01 and 0.04, from core helium ignition until core collapse. Throughout their lifetime, some stellar models expose the ashes of helium burning. We propose that models that have nitrogen-rich envelopes are candidate WN stars, while models with a carbon-rich surface are candidate WC stars during core helium burning, and WO stars afterwards. We measure metallicity dependance of the total lifetime of our models and the duration of their evolutionary phases. We propose an analytic estimate of the wind optical depth to distinguish models of Wolf-Rayet stars from transparent-wind stripped-envelope stars, and find that the luminosity ranges at which WN, WC and WO type stars can exist is a strong function of metallicity. We find that all carbon-rich models produced in our grids have optically thick winds and match the luminosity distribution of observed populations. We construct population models and predict the numbers of transparent-wind stripped-envelope stars and Wolf-Rayet stars, and derive their number ratios at different metallicities. We find that as metallicity increases, the number of transparent-wind stripped-envelope stars decreases and the number of Wolf-Rayet stars increases. At high metallicities WC and WO type stars become more common. We apply our population models to nearby galaxies, and find that populations are more sensitive to the transition luminosity between Wolf-Rayet stars and transparent-wind helium stars than to the metallicity dependent mass loss rates.

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Section: Comparison To Previous Stellar Evolution Modelssupporting

confidence: 80%

Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Aguilera-Dena,

Langer,

Antoniadis

et al. 2021

Preprint

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“…Spectral synthesis that distinguishes velocities of individual elements will also provide an alternative method to lift the degeneracy. Dessart et al (2020) showed that a star with no H-rich envelope explodes as a Type Ib (Ic) SN depending on its X(He) at the photosphere. According to Table 3 and Figure 3 in that work, a star with a photospheric He mass fraction X(He)  0.2 explodes as a Type Ic and X(He)  0.5 as a Type Ib SN.…”

Section: Light-curve Degeneraciesmentioning

confidence: 99%

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

Leung

Fuller

Nomoto

2021

ApJ

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The discovery of SN 2018gep (ZTF 18abukavn) challenged our understanding of the late-phase evolution of massive stars and their supernovae (SNe). The fast rise in luminosity of this SN (spectroscopically classified as a broad-lined Type Ic SN) indicates that the ejecta interacts with a dense circumstellar medium (CSM), while an additional energy source such as 56 Ni decay is required to explain the late-time light curve. These features hint at the explosion of a massive star with pre-SN mass loss. In this work, we examine the physical origins of rapidly evolving astrophysical transients like SN 2018gep. We investigate the wave-driven mass-loss mechanism and how it depends on model parameters such as progenitor mass and deposition energy, searching for stellar progenitor models that can reproduce the observational data. A model with an ejecta mass ∼2 M e , explosion energy ∼10 52 erg, a CSM of mass ∼0.3 M e and radius ∼1000 R e , and a 56 Ni mass ∼0.3 M e provides a good fit to the bolometric light curve. We also examine how interaction-powered light curves depend more generally on these parameters and how ejecta velocities can help break degeneracies. We find both wave-driven mass loss and mass ejection via pulsational pair instability can plausibly create the dense CSM in SN 2018gep, but we favor the latter possibility.

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“…Thus, these authors seem less keen to lean on the magnetar solution, even though they acknowledge that a sizeable fraction of the SE SNe might be out of reach (too bright) for their models. Woosley et al (2021) also occasionally discussed observational uncertainties, such as whether some specific SNe might have had their host extinction overestimated (see also Dessart et al 2020) or whether some are really "normal" Type Ibc SNe. They also ask whether the bolometric light curves (LCs) have been improperly assembled or if overly simplistic modeling was used to derive the amount of radioactive nickel.…”

Section: Introductionmentioning

confidence: 99%

Maximum luminosities of normal stripped-envelope supernovae are brighter than explosion models allow

Sollerman

Yang

Perley

et al. 2022

A&A

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Context. Stripped-envelope supernovae (SE SNe) of Type Ib and Type Ic are thought to be the result of explosions of massive stars that have lost their outer envelopes. The favored explosion mechanism is via core-collapse, with the shock later revived by neutrino heating. However, there is an upper limit to the amount of radioactive 56Ni that such models can accommodate. Recent studies in the literature point to a tension between the maximum luminosity from such simulations and the observations. Aims. We used a well-characterized sample of SE SNe from the Zwicky Transient Facility (ZTF) Bright Transient Survey (BTS) to scrutinize the observational caveats regarding estimates of the maximum luminosity (and thus the amount of ejected radioactive nickel) for the sample members. Methods. We employed the strict selection criteria for the BTS to collect a sample of spectroscopically classified normal Type Ibc SNe, for which we used the ZTF light curves to determine the maximum luminosity. We culled the sample further based on data quality, shape of the light curves, distances, and colors. Then we examined the uncertainties that may affect the measurements. The methodology of the sample construction based on this BTS sample can be used for other future investigations. Results. We analyzed the observational data, consisting of optical light curves and spectra, for the selected sub-samples. In total, we used 129 Type Ib or Type Ic BTS SNe with an initial rough luminosity distribution peaking at Mr = −17.61 ± 0.72, and where 36% are apparently brighter than the theoretically predicted maximum brightness of Mr = −17.8. When we further culled this sample to ensure that the SNe are normal Type Ibc with good LC data within the Hubble flow, the sample of 94 objects gives Mr = −17.64 ± 0.54. A main uncertainty in absolute magnitude determinations for SNe is the host galaxy extinction correction, but the reddened objects only get more luminous after corrections. If we simply exclude red objects, or those with unusual or uncertain colors, then we are left with 14 objects at Mr = −17.90 ± 0.73, whereof a handful are most certainly brighter than the suggested theoretical limit. The main result of this study is thus that normal SNe Ibc do indeed reach luminosities above 1042.6 erg s−1, which is apparently in conflict with existing explosion models.

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Supernovae Ib and Ic from the explosion of helium stars

Cited by 54 publications

References 120 publications

Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

Maximum luminosities of normal stripped-envelope supernovae are brighter than explosion models allow

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