The strongly interacting binary scenarios of the enigmatic supernova iPTF14hls

Gofman, Roni Anna; Soker, Noam

doi:10.1093/mnras/stz2179

Cited by 12 publications

(7 citation statements)

References 48 publications

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“…They further estimate the mass in the CSM to be ≈ 0.004 − 0.014M and the mass loss rate from the progenitor that formed this CSM to be ≈ 0.01 − 0.05M yr −1 . If indeed the CSM is in a torus, this geometry suggests a strong binary interaction (e.g., Gofman & Soker 2019) that probably spun-up the progenitor. With rapid rotation the stellar progenitor might be able to lift a dense equatorial effervescent zone with the required mass.…”

Section: An Example Of Velocity Distributionmentioning

confidence: 99%

A pre-explosion extended effervescent zone around core collapse supernova progenitors

Soker

2020

Preprint

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I propose a scenario according to which the dense compact circumstellar matter (CSM) that the ejecta of many core collapse supernovae (CCSNe) collide with within several days after explosion results from a dense zone where in addition to the stellar wind there is gas that does not reach the escape velocity. In this effervescent zone above red supergiant (RSG) stars, there are dense clumps that are ejected from the vicinity of the RSG surface, rise to radii of tens of astronomical units, and then fall back. I consider two simple velocity distributions of the ejected clumps. I find that the density of the bound mass can be tens of times that of the escaping wind, and therefore can mimic a very high mass loss rate. The dense effervescent CSM zone can (1) explain the collision of the ejecta of many CCSNe with a dense CSM days after explosion, (2) facilitate very high mass loss rate if the star experiences powerful pre-explosion activity, (3) form dust that obscures the progenitor in the visible band, and (4) lead to an efficient mass transfer to a stellar companion at separations of tens of astronomical units, if exists. The effervescent zone might exist for thousands of years and more, and therefore the effervescent CSM model removes the requirement from many type II CCSN progenitors to experience a very strong outburst just years to months before explosion.

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Section: An Example Of Velocity Distributionmentioning

confidence: 99%

A pre-explosion extended effervescent zone around core collapse supernova progenitors

Soker

2020

Preprint

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“…Soker (2016Soker ( , 2017 argued that the newly born NS accreted the surrounding matter with a very high specific angular momentum, to form an accretion disk, and a jet is likely to be launched. Combining magnetar and jets activities may take place in some peculiar superluminous CCSNe (Gofman & Soker 2019).…”

Section: Light-curves Fittingmentioning

confidence: 99%

Magnetar-Driven Shock Breakout Revisited and Implications for Double-Peaked Type I Superluminous Supernovae

Liu,

Gao,

Wang

et al. 2021

Preprint

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The discovery of early bumps in some type-I superluminous supernovae (SLSNe-I) before the main peaks offers an important clue to their energy source mechanisms. In this paper, we updated an analytic magnetar-powered model for fitting the multi-band light curves of double-peaked SLSNe-I: the early bump is powered by magnetar-driven shock breakout thermal emission, and the main peak is powered by a radiative diffusion through the SN ejecta as in the standard magnetar-powered model. Generally, the diffusive luminosity is greater than the shock breakout luminosity at the early time, which makes the shock breakout bumps usually not clearly seen as observed. To obtain a clear doublepeaked light curve, inefficient magnetar heating at early times is required. This model is applied to three well-observed double-peaked SLSNe-I (i.e., SN2006oz, LSQ14bdq, and DES14Xtaz). We find that a relative massive SN ejecta with M ej 10.2 − 18.1M and relative large kinetic energy of SN ejecta E sn (3.8 − 6.5) × 10 51 erg are required, and the thermalization efficiency of the magnetar heating is suppressed before t delay , which are in the range of 15 − 43 days. The model can well reproduce the observed light curves, with a reasonable and similar set of physical parameters for both the early bump and the main peak, strengthening support for magnetar-powered model. In the future, modeling of the double-peaked SLSNe-I will become more feasible as more events are discovered before the early bump.

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“…However, in the case of main sequence stars or giant stars, it is not easy to come up with a scenario of a fast spherical ejection event that runs into a disk. In any case, the collision of the fast ejecta with the equatorial outflow thermalizes only a fraction of h/r, where h is the half-thickness of the equatorial outflow at distance r. Metzger, & Pejcha (2017) use h/r = 0.3 in their study, and Gofman, & Soker (2019) find that they require a value of h/r 0.2 to explain the luminosity of the supernova iPTF14hls by ejecta-torus interaction.…”

Section: Polar Interaction Versus Equatorial Interactionmentioning

confidence: 99%

“…Another way to transfer kinetic energy to radiation is the collision of a spherical fast ejecta with an equatorial disk or an equatorial outflow (e.g., Andrews, & Smith 2018;Kurfürst & Krtička 2019), where the a binary interaction forms the equatorial mass concentration (e.g., Pejcha et al 2016a,b;Andrews, & Smith 2018;Hubová, & Pejcha 2019;Kurfürst & Krtička 2019;Gofman, & Soker 2019). I compare these cases to jet-powered radiation ILOTs in section 6.…”

Section: Introductionmentioning

confidence: 99%

Efficiently Jet-powered Radiation in Intermediate-luminosity Optical Transients

Soker

2020

ApJ

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I show that a flow structure where wide jets hit a slower expanding shell might be very efficient in channelling the kinetic energy of the jets to radiation, therefore accounting for, at a least a fraction of, intermediate luminosity optical transients (ILOTs) where the total radiation energy is much larger than what recombination energy of the outflow can supply. This type of flow might occur in the frame of the high-accretion-powered ILOT (HAPI) model, where there is a high mass accretion rate as a result of stellar merger or mass transfer in a binary system. I derive the condition on the jets halfopening angle for the jets not to penetrate through the slow shell, as well as the ratio of the photon diffusion time to expansion time. This ratio cannot be too large if a large fraction of the thermal energy is channelled to radiation. I apply the jet-powered radiation model to the Great Eruption of Eta Carinae, to V838 Mon, and to V4332 Sgr, and find a plausible set of parameters for these ILOTs. I expect the jet-powered radiation model to be more efficient in converting kinetic energy to radiation than ILOT models that are based on equatorial mass concentration. In many cases, thought, I expect both jets and equatorial mass concentration to occur in the same system.

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The strongly interacting binary scenarios of the enigmatic supernova iPTF14hls

Cited by 12 publications

References 48 publications

A pre-explosion extended effervescent zone around core collapse supernova progenitors

A pre-explosion extended effervescent zone around core collapse supernova progenitors

Magnetar-Driven Shock Breakout Revisited and Implications for Double-Peaked Type I Superluminous Supernovae

Efficiently Jet-powered Radiation in Intermediate-luminosity Optical Transients

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