Observational properties of low-redshift pair instability supernovae

Kozyreva, Alexandra; Блинников, С. И.; Langer, N.; Yoon, Sung‐Chul

doi:10.1051/0004-6361/201423447

Cited by 76 publications

(83 citation statements)

References 96 publications

(134 reference statements)

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“…A&A 581, A15 (2015) supernovae (Quimby et al 2011;Lunnan et al 2013) occur preferentially in low-metallicity dwarf galaxies. This may corroborate the idea that reduced wind mass-loss at low metallicity (Vink et al 2001;Mokiem et al 2007) may allow for rapid rotation rates (Yoon et al 2006;Georgy et al 2009) and very massive Yusof et al 2013;Kozyreva et al 2014) supernova progenitors. A good understanding of the evolution of metal-poor massive stars is, therefore, important to probe the origin of these extremely energetic explosions.…”

Section: Introductionsupporting

confidence: 74%

Low-metallicity massive single stars with rotation

Szécsi

Langer

Yoon

et al. 2015

A&A

152

213

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Context. Low-metallicity environments such as the early Universe and compact star-forming dwarf galaxies contain many massive stars. These stars influence their surroundings through intense UV radiation, strong winds and explosive deaths. A good understanding of low-metallicity environments requires a detailed theoretical comprehension of the evolution of their massive stars. Aims. We aim to investigate the role of metallicity and rotation in shaping the evolutionary paths of massive stars and to provide theoretical predictions that can be tested by observations of metal-poor environments. Methods. Massive rotating single stars with an initial metal composition appropriate for the dwarf galaxy I Zw 18 ([Fe/H] = −1.7) are modelled during hydrogen burning for initial masses of 9−300 M and rotational velocities of 0−900 km s −1 . Internal mixing processes in these models were calibrated based on an observed sample of OB-type stars in the Magellanic Clouds. Results. Even moderately fast rotators, which may be abundant at this metallicity, are found to undergo efficient mixing induced by rotation resulting in quasi chemically-homogeneous evolution. These homogeneously-evolving models reach effective temperatures of up to 90 kK during core hydrogen burning. This, together with their moderate mass-loss rates, make them transparent wind ultraviolet intense stars (TWUIN star), and their expected numbers might explain the observed He II ionising photon flux in I Zw 18 and other low-metallicity He II galaxies. Our slowly rotating stars above ∼80 M evolve into late B-to M-type supergiants during core hydrogen burning, with visual magnitudes up to 19 m at the distance of I Zw 18. Both types of stars, TWUIN stars and luminous late-type supergiants, are only predicted at low metallicity. Conclusions. Massive star evolution at low metallicity is shown to differ qualitatively from that in metal-rich environments. Our grid can be used to interpret observations of local star-forming dwarf galaxies and high-redshift galaxies, as well as the metal-poor components of our Milky Way and its globular clusters.

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Section: Introductionsupporting

confidence: 74%

Low-metallicity massive single stars with rotation

Szécsi

Langer

Yoon

et al. 2015

A&A

152

213

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“…This is because its light-curve (LC) decline rate after the LC peak is consistent with the nuclear decay rate of 56 Co and strong nebular Fe emission lines are also observed, as expected in PISNe (e.g., Kasen et al 2011;Dessart et al 2013;Kozyreva et al 2014;Whalen et al 2014;Chatzopoulos et al 2015).…”

supporting

confidence: 72%

“…7 are too short to correspond to PISNe (Kasen et al 2011;Dessart et al 2013;Kozyreva et al 2014;Chatzopoulos et al 2015 but see also Kozyreva et al 2016). On the contrary, many slowlydeclining SLSNe have decline rates which are surprisingly similar to that of the 56 Co decay as discussed in Section 1.…”

Section: Magnetar Vsmentioning

confidence: 99%

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

Moriya

Chen

Langer

2017

ApJ

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Many Type Ic superluminous supernovae have light-curve decline rates after their luminosity peak which are close to the nuclear decay rate of 56 Co, consistent with the interpretation that they are powered by 56 Ni and possibly pair-instability supernovae. However, their rise times are typically shorter than those expected from pair-instability supernovae, and Type Ic superluminous supernovae are often suggested to be powered by magnetar spin-down. If magnetar spin-down is actually a major mechanism to power Type Ic superluminous supernovae, it should be able to produce decline rates similar to the 56 Co decay rate rather easily. In this study, we investigate the conditions for magnetars under which their spin-down energy input can behave like the 56 Ni nuclear decay energy input. We find that an initial magnetic field strength within a certain range is sufficient to keep the magnetar energy deposition within a factor of a few of the 56 Co decay energy for several hundreds of days. Magnetar spin-down needs to be by almost pure dipole radiation with the braking index close to 3 to mimic 56 Ni in a wide parameter range. Not only late-phase 56 Co-decay-like light curves, but also rise time and peak luminosity of most 56 Ni-powered light curves can be reproduced by magnetars. Bolometric light curves for more than 700 days are required to distinguish the two energy sources solely by them. We expect that more slowly-declining superluminous supernovae with short rise times should be found if they are mainly powered by magnetar spin-down.

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“…Much work has been dedicated to modelling the appearance of PISNe during the shock breakout and diffusion phases (Kasen, Woosley & Heger 2011;Dessart et al 2012;Whalen et al 2013a;Dessart et al 2013;Chatzopoulos, Wheeler & Couch 2013;Whalen et al 2014;Smidt et al 2015;Chatzopoulos et al 2015;Kozyreva & Blinnikov 2015), and fitting of these models to observed candidates. The ability of central engine (magnetar spin-down or accreting black hole, Kasen & Bildsten 2010;Woosley 2010;Dexter & Kasen 2013) and circumstellar interaction (Smith et al 2007;Chevalier & Irwin 2011;Ginzburg & Balberg 2012) models to produce similar light curves has, however, left interpretation of observed long-duration events ambiguous Nicholl et al 2013;Moriya et al 2013;McCrum et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Nebular spectra of pair-instability supernovae

Jerkstrand

Smartt

Heger

2015

Mon. Not. R. Astron. Soc.

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If very massive stars (M 100 M ⊙ ) can form and avoid too strong mass loss during their evolution, they are predicted to explode as pair-instability supernovae (PISNe). One critical test for candidate events is whether their nucleosynthesis yields and internal ejecta structure, being revealed through nebular-phase spectra at t 1 yr, match those of model predictions. Here we compute theoretical spectra based on model PISN ejecta at 1-3 years post-explosion to allow quantitative comparison with observations. The high column densities of PISNe lead to complete gamma-ray trapping for t 2 years which, combined with fulfilled conditions of steady state, leads to bolometric supernova luminosities matching the 56 Co decay. Most of the gamma-rays are absorbed by the deep-lying iron and silicon/sulphur layers. The ionization balance shows a predominantly neutral gas state, which leads to emission lines of Fe I, Si I, and S I. For low-mass PISNe the metal core expands slowly enough to produce a forest of distinct lines, whereas high-mass PISNe expand faster and produce more featureless spectra. Line blocking is complete below ∼5000Å for several years, and the model spectra are red. The strongest line is typically [Ca II] λλ7291, 7323, one of few lines from ionized species. We compare our models with proposed PISN candidates SN 2007bi and PTF12dam, finding discrepancies for several key observables and thus no support for a PISN interpretation. We discuss distinct spectral features predicted by the models, and the possibility of detecting pair-instability explosions among non-superluminous supernovae.

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Observational properties of low-redshift pair instability supernovae

Cited by 76 publications

References 96 publications

Low-metallicity massive single stars with rotation

Low-metallicity massive single stars with rotation

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

Nebular spectra of pair-instability supernovae

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Observational properties of low-redshift pair instability supernovae

Cited by 76 publications

References 96 publications

Low-metallicity massive single stars with rotation

Low-metallicity massive single stars with rotation

Properties of Magnetars Mimicking 56Ni-Powered Light Curves in Type IC Superluminous Supernovae

Nebular spectra of pair-instability supernovae

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Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae