Supernova lightCURVE POPulation Synthesis I: Including interacting binaries is key to understanding the diversity of type II supernova lightcurves

Eldridge, J. J.; Xiao, Lin; Stanway, Elizabeth R.; Rodrigues, Nathalia Oliveira; Guo, Nan

doi:10.1017/pasa.2018.47

Cited by 43 publications

(49 citation statements)

References 56 publications

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“…This is particularly important if the binary fraction is high (Zapartas et al 2019). Additionally, Eldridge et al (2018) find that SN II-P like light curves can be produced from RSGs with M fin ∼ 4M , and that stellar mergers can produce RSGs with M fin ∼ 40M . For single stars, there is a much narrower expected range of final masses.…”

Section: Discussionmentioning

confidence: 90%

“…Our models predict that for a star to be a RSG at the end of its evolution (assuming T eff < 5000 K), it must have M env of 0.1−0.5M , depending on the value of M He-core . Eldridge et al (2018) found that the minimum hydrogen mass required to produce a SN II-P is 1M . RSGs with M env of ∼ 0.1 − 1M may produce SN II-L when they explode.…”

Section: Discussionmentioning

confidence: 99%

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The uncertain masses of progenitors of core-collapse supernovae and direct-collapse black holes

Farrell

Groh

Meynet

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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We show that it is not possible to determine the final mass M fin of a red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity L and effective temperature T eff alone. Using a grid of stellar models, we demonstrate that for a given value of L and T eff , a RSG can have a range of M fin as wide as 3 to 45 M . While the probability distribution within these limits is not flat, any individual determination of M fin for a RSG will be degenerate. This makes it difficult to determine its evolutionary history and to map M fin to an initial mass. Single stars produce a narrower range that is difficult to accurately determine without making strong assumptions about mass loss, convection, and rotation. Binaries would produce a wider range of RSG M fin . However, the final Helium core mass M He-core is well determined by the final luminosity and we find log(M He-core /M ) = 0.659 log(L/L ) − 2.630. Using this relationship, we derive M He-core for directly imaged SN progenitors and one failed SN candidate. The value of M fin for stripped star progenitors of SNe IIb is better constrained by L and T eff due to the dependence of T eff on the envelope mass M env for M env 1 M . Given the initial mass function, our results apply to the majority of progenitors of core collapse SNe, failed SNe and direct collapse black holes.

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Section: Discussionmentioning

confidence: 90%

Section: Discussionmentioning

confidence: 99%

The uncertain masses of progenitors of core-collapse supernovae and direct-collapse black holes

Farrell

Groh

Meynet

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…For massive stars, the main sequence phase is followed by the red supergiant phase, which is dominated by slow, dense winds, with velocities of ∼ 10-20 km s −1 and mass loss rates of ∼ 0.5-2.0 × 10 −5 M yr −1 (Smith 2014). While there are currently large uncertainties about the mass loss rates of RSGs based on observations (Georgy 2017), it is believed that most of the progenitor's mass is lost during the RSG phase, which lasts for 1.0 Myr (Eldridge et al 2018). The RSG wind expands into the low density main sequence wind, eventually forming a wind-blown, radiatively cooled shell.…”

Section: Cas A's Progenitor Mass-loss Historymentioning

confidence: 99%

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Weil

Fesen

Patnaude

et al. 2020

ApJ

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Cassiopeia A (Cas A) is one of the best studied young Galactic supernova remnants. While providing a rare opportunity to study in detail the remnant of a Type IIb supernova, questions remain regarding the nature of its progenitor, its mass-loss history, and its pre-SN evolution. Here we present an optical investigation of the circumstellar environment around Cas A and find clumpy and filamentary Hα emission nebulosities concentrated 10-15 pc (10-15 arcminutes) to the north and east. First reported by Minkowski as a faint H II region, these nebulosities exhibit distinct morphological and spectroscopic properties relative to the surrounding diffuse emissions. Compared to neighboring H II regions, these nebulae show stronger [N II] 6548, 6583Å and [S II] 6716, 6731Å emissions relative to Hα. We show that Cas A's highest-velocity ejecta knots are interacting with some of the closest projected emission nebulae, thus providing strong evidence that these nebulae lie at the same distance as the remnant. We interpret these surrounding nebulosities to be the remains of the progenitor's red supergiant wind which accumulated against the southern edge of a large extended H II region located north of Cas A. Our findings are consistent with the view that Cas A's progenitor underwent considerable mass-loss, first from a fast main-sequence wind, then from a slower, clumpy red supergiant wind, and finally from a brief high-velocity wind, like that from a yellow supergiant.

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“…However, there are few studies that focus on a quantitative comparison of light-curve morphologies between SNe II and SNe IIb (c.f. : Arcavi et al 2012, Faran et al 2014, Eldridge et al 2018).…”

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confidence: 99%

Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae

Pessi

Folatelli

Anderson

et al. 2019

Monthly Notices of the Royal Astronomical Society

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ABSTRACT Type II supernovae (SNe II) show strong hydrogen features in their spectra throughout their whole evolution, while type IIb supernovae (SNe IIb) spectra evolve from dominant hydrogen lines at early times to increasingly strong helium features later on. However, it is currently unclear whether the progenitors of these SN types form a continuum in pre-SN hydrogen mass or whether they are physically distinct. SN light-curve morphology directly relates to progenitor and explosion properties such as the amount of hydrogen in the envelope, the pre-SN radius, the explosion energy, and the synthesized mass of radioactive material. In this work, we study the morphology of the optical-wavelength light curves of hydrogen-rich SNe II and hydrogen-poor SNe IIb to test whether an observational continuum exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe IIb), we define a range of key observational parameters and present a comparative analysis between both types. We find a lack of events that bridge the observed properties of SNe II and IIb. Light-curve parameters such as rise times and post-maximum decline rates and curvatures clearly separate both SN types and we therefore conclude that there is no continuum, with the two SN types forming two observationally distinct families. In the V band a rise time of 17 d (SNe II lower and SNe IIb higher), and a magnitude difference between 30 and 40 d post-explosion of 0.4 mag (SNe II lower and SNe IIb higher) serve as approximate thresholds to differentiate both types.

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Supernova lightCURVE POPulation Synthesis I: Including interacting binaries is key to understanding the diversity of type II supernova lightcurves

Cited by 43 publications

References 56 publications

The uncertain masses of progenitors of core-collapse supernovae and direct-collapse black holes

The uncertain masses of progenitors of core-collapse supernovae and direct-collapse black holes

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae

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