Mass-loss histories of Type IIn supernova progenitors within decades before their explosion

Moriya, Takashi J.; Maeda, Keiichi; Taddia, F.; Sollerman, J.; Блинников, С. И.; Sorokina, E. I.

doi:10.1093/mnras/stu163

Cited by 113 publications

(101 citation statements)

References 60 publications

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“…The ecSN progenitors should be within the circumstellar medium (CSM) created by the super-AGB wind when they explode if they are single stars. In addition to the high mass-loss rates, the wind velocities of super-AGB stars are ∼10 km s −1 , making the CSM density as high as those expected for Type IIn SNe (SNe IIn) in which we see the effect of the CSM interaction in their observational properties (e.g., Kiewe et al 2012;Taddia et al 2013;Fransson et al 2013;Moriya et al 2014;see Sect. 2.1.2).…”

Section: Introductionmentioning

confidence: 83%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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The most massive stars on the asymptotic giant branch (AGB), or the so-called super-AGB stars, are thought to produce supernovae triggered by electron captures in their degenerate O+Ne+Mg cores. Super-AGB stars are expected to have slow winds with high mass-loss rates, so their circumstellar density is high. The explosions of super-AGB stars are therefore presumed to occur in this dense circumstellar environment. We provide the first synthetic light curves for such events by exploding realistic electron-capture supernova progenitors within their super-AGB winds. We find that the early light curve -that is, before the recombination wave reaches the bottom of the hydrogen-rich envelope of supernova ejecta (the plateau phase) -is not affected by the dense wind. However, after the luminosity drop following the plateau phase, the luminosity remains much higher when the super-AGB wind is taken into account. We compare our results to the historical light curve of SN 1054, the progenitor of the Crab Nebula, and show that the explosion of an electron-capture supernova within an ordinary super-AGB wind can explain the observed light curve features. We conclude that SN 1054 could have been a Type IIn supernova without any extra extreme mass loss, which was previously suggested to be necessary to account for its early high luminosity. We also show that our light curves match Type IIn supernovae with an early plateau phase or the so-called Type IIn-P supernovae, and suggest that they are electron-capture supernovae within super-AGB winds. Although some electron-capture supernovae can be bright in the optical spectral range due to the large progenitor radius, their X-ray luminosity from the interaction does not necessarily get as bright as other Type IIn supernovae whose optical luminosities are also powered by the interaction. Thus, we suggest that optically bright X-ray-faint Type IIn supernovae can emerge from electron-capture supernovae. Optically faint Type IIn supernovae, such as SN 2008S, can also originate from electron-capture supernovae if their hydrogen-rich envelope masses are small. We argue that some of them can be observed as Type IIn-b supernovae due to the small hydrogen-rich envelope mass.

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Section: Introductionmentioning

confidence: 83%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

Self Cite

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“…It seems that the pre-explosion outbursts of CCSNe are common (e.g., Moriya et al 2014;Ofek et al 2014;Svirski & Nakar 2014;Tartaglia et al 2016;Yaron et al 2017), with about one in ten CCSNe suffering a pre-explosion outburst (e.g., Margutti et al 2017). The outburst might result from a single-star process, e.g., strong convection in the pre-collapsing core (Quataert & Shiode 2012;Shiode & Quataert 2014).…”

Section: Observational Consequencesmentioning

confidence: 99%

The two promising scenarios to explode core collapse supernovae

Soker

2017

Res. Astron. Astrophys.

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I compare to each other what I consider to be the two most promising scenarios to explode core-collapse supernovae (CCSNe). Both are based on the negative jet feedback mechanism (JFM). In the jittering jets scenario a collapsing core of a single slowly-rotating star can launch jets. The accretion disk or belt (a sub-Keplerian accretion flow concentrated toward the equatorial plane) that launches the jets is intermittent with varying directions of the axis. Instabilities, such as the standing accretion shock instability (SASI), lead to stochastic angular momentum variations that allow the formation of the intermittent accretion disk/belt. According to this scenario no failed CCSNe exist. According to the fixed axis scenario, the core of the progenitor star must be spun up during its late evolutionary phases, and hence all CCSNe are descendants of strongly interacting binary systems, most likely through a common envelope evolution (whether the companion survives or not). Due to the strong binary interaction, the axis of the accretion disk that is formed around the newly born neutron star has a more or less fixed direction. According to the fixed axis scenario, accretion disk/belt are not formed around the newly born neutron star of single stars; they rather end in failed CCSNe. I also raise the possibility that the jittering jets scenario operates for progenitors with initial mass of 8M ⊙ M ZAMS 18M ⊙ , while the fixed axis scenario operates for M ZAMS 18M ⊙ . For the first time these two scenarios are compared to each other, as well as to some aspects of neutrino-driven explosion mechanism. These new comparisons further suggest that the JFM plays a major role in exploding massive stars.

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“…Indeed, both SN IIn (Kiewe et al 2012;Ofek et al 2013;Moriya et al 2014) and IIb SNe, such as 2013cu (Gal-Yam et al 2014;Groh 2014;Gräfener & Vink 2016) seem to have been subjected to increased mass loss prior to explosion. This increased mass loss is oftentimes attributed to "eruptive" mass loss (Smith 2015), although a physical mechanism for such eruptive mass loss has not been agreed upon.…”

Section: Introductionmentioning

confidence: 99%

Two bi-stability jumps in theoretical wind models for massive stars and the implications for luminous blue variable supernovae

Petrov¹,

Gräfener²

2016

Mon. Not. R. Astron. Soc.

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Luminous Blue Variables have been suggested to be the direct progenitors of supernova types IIb and IIn, with enhanced mass loss prior to explosion. However, the mechanism of this mass loss is not yet known. Here, we investigate the qualitative behaviour of theoretical stellar wind mass-loss as a function of T eff across two bi-stability jumps in blue supergiant regime and also in proximity to the Eddington limit, relevant for LBVs. To investigate the physical ingredients that play a role in the radiative acceleration we calculate blue supergiant wind models with the cmfgen non-LTE model atmosphere code over an effective temperature range between 30 000 and 8 800 K. Although our aim is not to provide new mass-loss rates for BA supergiants, we study and confirm the existence of two bi-stability jumps in mass-loss rates predicted by Vink, de Koter, & Lamers (1999). However, they are found to occur at somewhat lower T eff (20 000 and 9 000 K, respectively) than found previously, which would imply that stars may evolve towards lower T eff before strong mass-loss is induced by the bistability jumps. When the combined effects of the second bi-stability jump and the proximity to Eddington limit are accounted for, we find a dramatic increase in the mass-loss rate by up to a factor of 30. Further investigation of both bi-stability jumps is expected to lead to a better understanding of discrepancies between empirical modelling and theoretical mass-loss rates reported in the literature, and to provide key inputs for the evolution of both normal AB supergiants and LBVs, as well as their subsequent supernova type II explosions.

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Mass-loss histories of Type IIn supernova progenitors within decades before their explosion

Cited by 113 publications

References 60 publications

Electron-capture supernovae exploding within their progenitor wind

Electron-capture supernovae exploding within their progenitor wind

The two promising scenarios to explode core collapse supernovae

Two bi-stability jumps in theoretical wind models for massive stars and the implications for luminous blue variable supernovae

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