Pulsational Pair-instability Supernovae

Woosley, S. E.

doi:10.3847/1538-4357/836/2/244

Cited by 716 publications

(859 citation statements)

References 151 publications

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“…This would require some mechanisms that can eject multiple layers of material from massive progenitor stars within a time interval of several decades before supernova explosion. One possibility is Pulsational Pair-instability supernova (Woosley 2017). Quantitative modelings of our data are needed.…”

Section: Discussionmentioning

confidence: 99%

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Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Yan

Lunnan

Perley

et al. 2017

ApJ

123

134

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We present observations of two new hydrogen-poor superluminous supernovae (SLSN-I), iPTF15esb and iPTF16bad, showing late-time Hα emission with line luminosities of 1 3 10 41 ( -) erg s −1 and velocity widths of (4000-6000) km s −1 . Including the previously published iPTF13ehe, this makes up a total of three such events to date. iPTF13ehe is one of the most luminous and the slowest evolving SLSNe-I, whereas the other two are less luminous and fast decliners. We interpret this as a result of the ejecta running into a neutral H-shell located at a radius of ∼10 16 cm. This implies that violent mass loss must have occurred several decades before the supernova explosion. Such a short time interval suggests that eruptive mass loss could be common shortly before core collapse, and more importantly helium is unlikely to be completely stripped off the progenitor and could be present in the ejecta. It is a mystery why helium features are not detected, even though nonthermal energy sources, capable of ionizing He, may exist as suggested by the O II absorption series in the early-time spectra. Our late-time spectra (+240 days) appear to have intrinsically lower [O I] 6300 Å luminosities than that of SN2015bn and SN2007bi, which is possibly an indication of less oxygen (<10 M e ). The blueshifted Hα emission relative to the hosts for all three events may be in tension with the binary model proposed for iPTF13ehe. Finally, iPTF15esb has a peculiar light curve (LC) with three peaks separated from one another by ∼22 days. The LC undulation is stronger in bluer bands. One possible explanation is ejecta-circumstellar medium interaction.

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Section: Discussionmentioning

confidence: 99%

“…The probability of these three events being PPISN or PISN is small. First is because the required progenitor mass is very high, and second, as pointed by Woosley (2017), PPISN still has difficulties producing very energetic SLSNe-I, and iPTF13ehe is such an example.…”

Section: Weak [O I] 6300 Doublet Emissionmentioning

confidence: 99%

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Yan

Lunnan

Perley

et al. 2017

ApJ

123

134

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“…Whether or not this produce some flashes or even an explosion in the presupernova phases remain to be explored. Recently, Woosley (2017) has investigated the final evolution of 70 − 140 M stars. He finds that such stars should experience Pulsational Pair Instability Supernovae (PPISN).…”

Section: Internal Structure Of the 85 And 120 M Modelsmentioning

confidence: 99%

Effects of axions on Population III stars

Choplin

Coc

Meynet

et al. 2017

A&A

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Aims. Following the renewed interest for axions as a dark matter component, we revisit the effects of energy loss by axion emission on the evolution of the first generation of stars. These stars with zero metallicity are supposed to be massive, more compact, and hotter than subsequent generations. It is hence important to extend previous studies restricted to solar metallicity stars. Methods. Our analysis first compares the evolution of solar metallicity 8, 10 and 12 M stars to previous work. We then calculate the evolution of 8 zero metallicity stars with and without axion losses and with masses ranging from 20 to 150 M . Results. For the solar metallicity models, we confirm the disappearance of the blue loop phase for a value of the axion-photon coupling, g aγ = 10−10 GeV −1 . Regarding the Pop. III stars, we show that for g aγ = 10 −10 GeV −1 , their evolution is not much affected by axion losses except within the range of masses 80-130 M . Such stars show significant differences both in their tracks within the T c -ρ c diagram and in their central composition (in particular 20 Ne and 24 Mg). We discuss the origin of these modifications from the stellar physics point of view, and their potential observational signatures.

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“…Observations of SNe IIn and superluminous SNe may perhaps be explained by the strong interaction between the SN shock and shells of material ejected from the star in late stages of its evolution, (e.g., Smith et al 2011;Smith 2014;Shiode & Quataert 2014). It has also been proposed that the coupling of mass loss and rotation might prevent pair instability SNe for very massive, low metallicity stars (Ekström et al 2008;Woosley 2017).…”

Section: Introductionmentioning

confidence: 99%

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

Renzo¹,

Ott²,

Shore³

et al. 2017

A&A

131

150

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Mass loss processes are a key uncertainty in the evolution of massive stars. They determine the amount of mass and angular momentum retained by the star, thus influencing its evolution and presupernova structure. Because of the high complexity of the physical processes driving mass loss, stellar evolution calculations must employ parametric algorithms, and usually only include wind mass loss. We carried out an extensive parameter study of wind mass loss and its effects on massive star evolution using the open-source stellar evolution code MESA. We provide a systematic comparison of wind mass loss algorithms for solar-metallicity, nonrotating, single stars in the initial mass range of 15 M to 35 M . We consider combinations drawn from two hot phase (i.e., roughly the main sequence) algorithms, three cool phase (i.e., post-main-sequence) algorithms, and two Wolf-Rayet mass loss algorithms. We discuss separately the effects of mass loss in each of these phases. In addition, we consider linear wind efficiency scale factors of 1, 0.33, and 0.1 to account for suggested reductions in mass loss rates due to wind inhomogeneities. We find that the initial to final mass mapping for each zero-age main-sequence (ZAMS) mass has a ∼50% uncertainty if all algorithm combinations and wind efficiencies are considered. The ad-hoc efficiency scale factor dominates this uncertainty. While the final total mass and internal structure of our models vary tremendously with mass loss treatment, final luminosity and effective temperature are much less sensitive for stars with ZAMS mass 30 M . This indicates that uncertainty in wind mass loss does not negatively affect estimates of the ZAMS mass of most single-star supernova progenitors from pre-explosion observations. Our results furthermore show that the internal structure of presupernova stars is sensitive to variations in both main sequence and post main-sequence mass loss. The compactness parameter ξ ∝ M/R(M) has been identified as a proxy for the "explodability" of a given presupernova model. We find that ξ varies by as much as 30% for models of the same ZAMS mass evolved with different wind efficiencies and mass loss algorithm combinations. This suggests that the details of the mass loss treatment might bias the outcome of detailed core-collapse supernova calculations and the predictions for neutron star and black hole formation.

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Pulsational Pair-instability Supernovae

Cited by 716 publications

References 151 publications

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Effects of axions on Population III stars

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

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