Optical and spectral observations and hydrodynamic modelling of type IIb supernova 2017gpn

Balakina, Elena; Pruzhinskaya, M.; Москвитин, А. С.; Блинников, С. И.; Xiang, Danfeng; Lin, Han; Rui, Liming; Wang, Huijuan

doi:10.1093/mnras/staa3383

“…The 56 Ni masses of SE SNe have also been computed through hydrodynamical modeling of light curves (e.g., Utrobin 1996;Nakamura et al 2001;Mazzali et al 2002;Sauer et al 2006;Tanaka et al 2009;Tsvetkov et al 2009;Bersten et al 2012Bersten et al , 2014Bufano et al 2014;Folatelli et al 2014;Ergon et al 2015;Folatelli et al 2015;Morales-Garoffolo et al 2015;Fremling et al 2016;Taddia et al 2016Taddia et al , 2018bBersten et al 2018;Balakina et al 2021). In particular, Taddia et al (2018b) found that the 56 Ni masses inferred with the Arnett model are consistent with those computed with the hydrodynamical models generated with the code of Bersten et al (2011).…”

Section: Introductionmentioning

confidence: 81%

The Iron Yield of Core-collapse Supernovae

Rodríguez,

Maoz,

Nakar

2023

ApJ

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We present a systematic analysis of 191 stripped-envelope supernovae (SE SNe), aimed at computing their 56Ni masses from the luminosity in their radioactive tails ( M Ni tail ) and/or in their maximum light, and the mean 56Ni and iron yields of SE SNe and core-collapse SNe. Our sample consists of SNe IIb, Ib, and Ic from the literature and from the Zwicky Transient Facility Bright Transient Survey. To calculate luminosities from optical photometry, we compute bolometric corrections using 49 SE SNe with optical and near-IR photometry, and develop corrections to account for the unobserved UV and IR flux. We find that the equation of Khatami & Kasen for radioactive 56Ni-powered transients with a single free parameter does not fit the observed peak time–luminosity relation of SE SNe. Instead, we find a correlation between M Ni tail , peak time, peak luminosity, and decline rate, which allows for measuring individual 56Ni masses to a precision of 14%. Applying this method to the whole sample, we find, for SNe IIb, Ib, and Ic, mean 56Ni masses of 0.066 ± 0.006, 0.082 ± 0.009, and 0.132 ± 0.011 M ⊙, respectively. After accounting for their relative rates, for SE SNe as a whole, we compute mean 56Ni and iron yields of 0.090 ± 0.005 and 0.097 ± 0.007 M ⊙, respectively. Combining these results with the recent Type II SN mean 56Ni mass derived by Rodríguez et al., core-collapse SNe, as a whole, have mean 56Ni and iron yields of 0.055 ± 0.006 and 0.058 ± 0.007 M ⊙, respectively. We also find that radioactive 56Ni-powered models typically underestimate the peak luminosity of SE SNe by 60%–70%, suggesting the presence of an additional power source contributing to the luminosity at peak.

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“…In Dessart et al (2018b), the radiation hydrodynamics (RHD) code v1d and the non-LTE radiative transport code CMFGEN were used for modeling the evolution of the ejecta and obtaining the optical light curves, respectively. Several studies adopted the STELLA code (Blinnikov et al 1998(Blinnikov et al , 2006Blinnikov & Tolstov 2011), a 1D RHD code that implicitly calculates the radiative transfer over multiple frequency bands, in order to generate spectral energy distributions (SEDs) and obtain optical light-curve models (see Tsvetkov et al 2009Tsvetkov et al , 2012Nakaoka et al 2019;Balakina et al 2021). Some studies assume that the SEDs from an SN are blackbody spectra of the effective temperature at the photosphere (usually defined by the Rosseland mean opacity) or a color temperature obtained from an analytical approximation (Bersten et al 2012;Piro et al 2017;Bersten et al 2018;Eldridge et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The Effects of Thomson Scattering and Chemical Mixing on Early-time Light Curves of Double-peaked Type IIb Supernovae

Park,

Yoon,

Blinnikov

2023

ApJ

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0

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Previous numerical simulations of double-peaked Type IIb supernova (SN IIb) light curves have demonstrated that the radius and mass of the hydrogen-rich envelope of the progenitor star can significantly influence the brightness and timescale of the early-time light curve around the first peak. In this study, we investigate how Thomson scattering and chemical mixing in the SN ejecta affect the optical light curves during the early stages of the SNe IIb using radiation hydrodynamics simulations. By comparing the results from two different numerical codes (i.e., STELLA and SNEC), we find that the optical brightness of the first peak can be reduced by more than a factor of 3 as a result of the effect of Thomson scattering that causes the thermalization depth to be located below the Rosseland mean photosphere, compared to the corresponding case where this effect is ignored. We also observe a short-lived plateau-like feature lasting for a few days in the early-time optical light curves of our models, in contrast to typical observed SNe IIb that show a quasi-linear decrease in optical magnitudes after the first peak. A significant degree of chemical mixing between the hydrogen-rich envelope and the helium core in SN ejecta is required to reconcile this discrepancy between the model prediction and observation. Meanwhile, to properly reproduce the first peak, a significant mixing of 56Ni into the hydrogen-rich outermost layers should be restricted. Our findings indicate that inferring the SN IIb progenitor structure from a simplified approach that ignores these two factors may introduce substantial uncertainty.

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“…The kinetic energy of SN 2019tua can be calculated, ∼0.5 × 10 51 erg. SN 2019tua has a lower kinetic energy compared to those of some Type IIb SNe, such as SN 2017gpn (∼3 × 10 51 erg;Balakina et al 2021), SN 2020acat (∼1.2 × 10 51 erg; Medler et al 2022), SN 2011fu (∼1.3 × 10 51 erg; Morales-Garoffolo et al 2015), ASASSN-14dq (∼1.24 × 10 51 erg; Singh et al 2018), SN 2020cxd…”

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confidence: 98%

SN 2019tua: A Type IIb Supernova with Multiple Bumps in the Light Curves

Huang,

Wang,

Li

et al. 2024

ApJ

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We present photometric and spectroscopic observations and analysis of the Type IIb supernova (SN) SN 2019tua, which exhibits multiple bumps in its declining light curves between 40 and 65 days after discovery. SN 2019tua shows a time to peak of about 25 days, similar to other Type IIb SNe. Our observations indicate a decrease in its brightness of about 1 mag in the 60 days after the peak. At about days 50 and 60, its multiband light curves exhibit bumpy behavior. The complex luminosity evolution of SN 2019tua could not be well modeled with a single currently popular energy source model, e.g., radioactive decay of 56Ni, magnetar, interaction between the ejecta and a circumstellar shell. Even though the magnetar model has a smaller χ 2/dof value, the complex changes in SN 2019tua’s brightness suggest that more than one physical process might be involved. We propose a hybrid circumstellar medium (CSM) interaction plus 56Ni model to explain the bolometric light curve of SN 2019tua. The fitting results show that the ejecta mass M ej ≈ 2.4 M ⊙, the total CSM mass M CSM ≈ 1.0 M ⊙, and the 56Ni mass M Ni ≈ 0.4 M ⊙. The total kinetic energy of the ejecta is E k ≈ 0.5 × 1051 erg. Preexisting multiple shells suggest that the progenitor of SN 2019tua experienced mass ejections within approximately ∼6–44 yr prior to the explosion.

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Optical and spectral observations and hydrodynamic modelling of type IIb supernova 2017gpn

Cited by 4 publications

References 68 publications

The Iron Yield of Core-collapse Supernovae

The Iron Yield of Core-collapse Supernovae

The Effects of Thomson Scattering and Chemical Mixing on Early-time Light Curves of Double-peaked Type IIb Supernovae

SN 2019tua: A Type IIb Supernova with Multiple Bumps in the Light Curves

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