The Circumstellar Material around the Type IIP SN 2021yja

Kozyreva, Alexandra; Klencki, J.; Filippenko, A. V.; Бакланов, П. В.; Миронов, А. П.; Justham, Stephen; Чиавасса, А.

doi:10.3847/2041-8213/ac835a

Cited by 11 publications

(7 citation statements)

References 82 publications

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“…An interesting paradox arises here. Morozova et al (2017), Morozova et al (2018), or Kozyreva et al (2022) argue for a large CSM mass of 0.5 M ⊙ (and an associated mass-loss rate of order 0.1 M ⊙ yr −1 ) in objects that have essentially standard type II-P SN luminosity of a few 10 42 erg s −1 . 6 The luminosity boost is small in those simulations because the density is so high that radiation cannot escape and therefore turns eventually mostly into kinetic energy.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…The most widely-accepted mechanism is a CSM that forms from a super-wind phase (Quataert & Shiode 2012;Fuller 2017) taking place in the months to years before core collapse (Morozova et al 2017;Moriya et al 2017;Dessart et al 2017;Morozova et al 2018). The ambiguity of the observables opens alternative possibilities, such as a progressive mass overloading taking place over the entire RSG lifetime, as proposed by Dessart et al (2017) or more recently Soker (2021), or RSG envelope convection and associated instabilities (Kozyreva et al 2022;Goldberg et al 2022a).…”

Section: Introductionmentioning

confidence: 99%

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Radiative-transfer modeling of nebular-phase type II supernovae

Dessart

Hillier

2020

A&A

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Nebular phase spectra of core-collapse supernovae (SNe) provide critical and unique information on the progenitor massive star and its explosion. We present a set of 1-D steady-state non-local thermodynamic equilibrium radiative transfer calculations of type II SNe at 300 d after explosion. Guided by results for a large set of stellar evolution simulations, we craft ejecta models for type II SNe from the explosion of a 12, 15, 20, and 25 M star. The ejecta density structure and kinetic energy, the 56 Ni mass, and the level of chemical mixing are parametrized. Our model spectra are sensitive to the adopted line Doppler width, a phenomenon we associate with the overlap of Fe ii and O i lines with Ly α and Ly β. Our spectra show a strong sensitivity to 56 Ni mixing since it determines where decay power is absorbed. Even at 300 d after explosion, the H-rich layers reprocess the radiation from the inner metal rich layers. In a given progenitor model, variations in 56 Ni mass and distribution impact the ejecta ionization, which can modulate the strength of all lines. Such ionization shifts can quench Ca ii line emission. In our set of models, the [O i] λλ 6300, 6364 doublet strength is the most robust signature of progenitor mass. However, we emphasize that convective shell merging in the progenitor massive star interior can pollute the O-rich shell with Ca, which will weaken the O i doublet flux in the resulting nebular SN II spectrum. This process may occur in Nature, with a greater occurrence in higher mass progenitors, and may explain in part the preponderance of progenitor masses below 17 M inferred from nebular spectra.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Radiative-transfer modeling of nebular-phase type II supernovae

Dessart

Hillier

2020

A&A

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“…The compilation of these UV spectra does not show the uniformity suggested by Gal-Yam et al (2008). In addition to the differences noted above for SN 1999em, SN 2021yja, and SN 2022wsp continue to show NUV flux out to 20 days, possibly due to weak interaction (Dessart & Hillier 2022;Hosseinzadeh et al 2022;Kozyreva et al 2022;Vasylyev et al 2023).…”

Section: Comparison To Other Early Uv Spectramentioning

confidence: 82%

SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova

Bostroem,

Dessart,

Hillier

et al. 2023

ApJL

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We present five far- and near-ultraviolet spectra of the Type II plateau supernova, SN 2022acko, obtained 5, 6, 7, 19, and 21 days after explosion, all observed with the Hubble Space Telescope/Space Telescope Imaging Spectrograph. The first three epochs are earlier than any Type II plateau supernova has been observed in the far-ultraviolet revealing unprecedented characteristics. These three spectra are dominated by strong lines, primarily from metals, which contrasts with the featureless early optical spectra. The flux decreases over the initial time series as the ejecta cool and line blanketing takes effect. We model this unique data set with the non–local thermodynamic equilibrium radiation transport code CMFGEN, finding a good match to the explosion of a low-mass red supergiant with energy E kin = 6 × 1050 erg. With these models we identify, for the first time, the ions that dominate the early ultraviolet spectra. We present optical photometry and spectroscopy, showing that SN 2022acko has a peak absolute magnitude of V = − 15.4 mag and plateau length of ∼115 days. The spectra closely resemble those of SN 2005cs and SN 2012A. Using the combined optical and ultraviolet spectra, we report the fraction of flux as a function of bluest wavelength on days 5, 7, and 19. We create a spectral time-series of Type II supernovae in the ultraviolet, demonstrating the rapid decline of flux over the first few weeks of evolution. Future observations of Type II supernovae are required to map out the landscape of exploding red supergiants, with and without circumstellar material, which is best revealed in high-quality ultraviolet spectra.

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“…We adopt the one-dimensional multi-frequency radiation hydrodynamics code STELLA to construct the model grid (Blinnikov et al 1998;Blinnikov et al 2000;Blinnikov et al 2006). STELLA has been used for Type II SN light-curve modeling intensively (e.g., Goldberg et al 2019;Hiramatsu et al 2021;Kozyreva et al 2022b for recent examples).…”

Section: Numerical Computationsmentioning

confidence: 99%

Synthetic red supergiant explosion model grid for systematic characterization of Type II supernovae

Moriya

Subrayan

Milisavljevic

et al. 2023

Publications of the Astronomical Society of Japan

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A new model grid containing 228016 synthetic red supergiant explosions (Type II supernovae) is introduced. Time evolution of spectral energy distributions from 1 to 50000 Å (100 frequency bins in a log scale) is computed at each time step up to 500 d after explosion in each model. We provide light curves for the filters of Vera C, Rubin Observatory’s Legacy Survey of Space and Time (LSST), the Zwicky Transient Facility, the Sloan Digital Sky Survey, and the Neil Gehrels Swift Observatory, but light curves for any photometric filters can be constructed by convolving any filter response functions to the synthetic spectral energy distributions. We also provide bolometric light curves and photosphere information such as photospheric velocity evolution. The parameter space covered by the model grid is five progenitor masses (10, 12, 14, 16, and 18 M$_{\odot}$ at the zero-age main sequence, solar metallicity), ten explosion energies (0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0 × 1051 erg), nine 56Ni masses (0.001, 0.01, 0.02, 0.04, 0.06, 0.08, 0.1, 0.2, and 0.3 M$_{\odot}$), nine mass-loss rates (10−5.0, 10−4.5, 10−4.0, 10−3.5, 10−3.0, 10−2.5, 10−2.0, 10−1.5, and 10−1.0 M$_{\odot}$ yr−1 with a wind velocity of 10 km s−1), six circumstellar matter radii (1, 2, 4, 6, 8, and 10 × 1014 cm), and ten circumstellar structures (β = 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0). 56Ni is assumed to be uniformly mixed up to the half-mass of a hydrogen-rich envelope. This model grid can be a base for rapid characterizations of Type II supernovae with sparse photometric sampling expected in LSST through a Bayesian approach, for example. The model grid is available at https://doi.org/10.5061/dryad.pnvx0k6sj.

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The Circumstellar Material around the Type IIP SN 2021yja

Cited by 11 publications

References 82 publications

Radiative-transfer modeling of nebular-phase type II supernovae

Radiative-transfer modeling of nebular-phase type II supernovae

SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova

Synthetic red supergiant explosion model grid for systematic characterization of Type II supernovae

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