Type IIb supernova progenitors by fatal common envelope evolution

Lohev, Noam; Sabach, Efrat; Gilkis, Avishai; Soker, Noam

doi:10.1093/mnras/stz2593

Cited by 19 publications

(19 citation statements)

References 64 publications

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“…A key question about SE SNe is the mechanisms that drive the removal of the envelopes of their progenitor stars. In particular, the debate centers around the relative roles, if any, of stellar winds (e.g., Woosley et al 1993;Georgy et al 2012;Groh et al 2013b), stellar rotation (e.g., Georgy et al 2012;Groh et al 2013a,b;Zhao & Fuller 2020), binary interactions (e.g., Podsiadlowski et al 1992;Yoon et al 2010Yoon et al , 2017Soker 2017;Lohev et al 2019), and, nuclear burning instabilities (e.g., Arnett & Meakin 2011;Strotjohann et al 2015). There has been growing support for binary interactions as dominant due to several independent lines of evidence, including weaker stellar winds (Smith 2014) and higher binary fractions (Sana et al 2012;Moe & Di Stefano 2017) than previously estimated.…”

Section: Introductionmentioning

confidence: 99%

Progenitors of Type IIb Supernovae. II. Observable Properties

Sravan

Marchant

Kalogera

et al. 2020

ApJ

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Type IIb supernovae (SNe IIb) present a unique opportunity for investigating the evolutionary channels and mechanisms governing the evolution of stripped-envelope SN progenitors due to a variety of observational constraints available. Comparison of these constraints with the full distribution of theoretical properties not only help ascertain the prevalence of observed properties in nature, but can also reveal currently unobserved populations. In this follow-up paper, we use the large grid of models presented in Sravan et al. (2019) to derive distributions of single and binary SNe IIb progenitor properties and compare them to constraints from three independent observational probes: multi-band SN light-curves, direct progenitor detections, and X-ray/radio observations. Consistent with previous work, we find that while current observations exclude single stars as SN IIb progenitors, SN IIb progenitors in binaries can account for them. We also find that the distributions indicate the existence of an unobserved dominant population of binary SNe IIb at low metallicity that arise due to mass transfer initiated on the Hertzsprung Gap. In particular, our models indicate the existence of a group of highly stripped (envelope mass ∼ 0.1 − 0.2M ) progenitors that are compact (< 50R ) and blue (T eff 10 5 K) with ∼ 10 4.5 − 10 5.5 L and low density circumstellar mediums. As discussed in Sravan et al. (2019), this group is necessary to account for SN IIb fractions and likely exist regardless of metallicity. The detection of the unobserved populations indicated by our models would support weak stellar winds and inefficient mass transfer in SN IIb progenitors.

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Section: Introductionmentioning

confidence: 99%

Progenitors of Type IIb Supernovae. II. Observable Properties

Sravan

Marchant

Kalogera

et al. 2020

ApJ

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“…10R are E bind (10R ) ≈ 10 47 − 10 49 erg, where the lower values are for RSG masses of M RSG ≈ 10M and radii of R RSG 10 3 R and the larger values are for RSG of M RSG ≈ 30M and R RSG 200R (e.g., Lohev et al 2019).…”

Section: Tight Binary System Inside the Rsg Envelopementioning

confidence: 99%

Double common envelope jets supernovae (CEJSNe) by triple-star systems

Soker

2021

Preprint

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I propose a new type of common envelope jets supernova (CEJSN) events where instead of a single neutron star (NS; or a black hole; BH) a tight binary system of a NS and a main sequence star enters a common envelope evolution (CEE) with a red supergiant. The NS and the main sequence star of the tight binary system merge inside the red supergiant envelope and enter a CEE of their own. The NS accretes some mass through an accretion disk and launches jets that explodes the main sequence star. I estimate that the two jets that the NS launches at this phase carry an energy of E 2j,4 ≈ 10 52 erg, about the same order of magnitude as the energy that the jets will carry when the NS or its BH remnant will enter the core in a later phase. For that, I term the entire event a double CEJSN. The outcome of the double CEJSN is a very long, months to years, and very energetic event, a total energy of ≈ 10 52 −10 53 erg, that will be observationally classified as a peculiar super-energetic event. I crudely estimate that new transient surveys should detect about one CEJSN event from a triple star system per year. I end by listing some other types of CEJSN events in triple star systems.

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“…In calculating the binding energy of the envelope that resides at r > 1R we took half the gravitational energy of that part of the envelope E env = 0.5|U grav |. At a radius of ≈ 1R the binding energy calculated this way and that calculated by adding the gravitational and internal energy become equal (e.g., Lohev et al 2019).…”

Section: Evolution To the Ceementioning

confidence: 99%

The future influence of six exoplanets on the envelope properties of their parent stars on the giant branches

Rapoport,

Bear,

Soker

2021

Preprint

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We study the evolution of six exoplanetary systems with the stellar evolutionary code mesa and conclude that they will likely spin-up the envelope of their parent stars on the red giant branch (RGB) or later on the asymptotic giant branch (AGB) to the degree that the mass loss process might become non-spherical. We choose six observed exoplanetary systems where the semi-major axis is a i 1−2 AU, and use the binary mode of mesa to follow the evolution of the systems. In four systems the star engulfs the planet on the RGB, and in two systems on the AGB, and the systems enter a common envelope evolution (CEE). In two systems where the exoplanet masses are M p 10M J , where M J is Jupiter mass, the planet spins-up the envelope to about 10% of the break-up velocity. Such envelopes are likely to have significant non-spherical mass loss geometry. In the other four systems where M p M J the planet spins-up the envelope to values of 1 − 2% of break-up velocity. Magnetic activity in the envelope that influences dust formation might lead to a small departure from spherical mass loss even in these cases. In the two cases of CEE on the AGB the planet deposits energy to the envelope that amounts to > 10% of the envelope binding energy. We expect this to cause a non-spherical mass loss that will shape an elliptical planetary nebula in each case.

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Type IIb supernova progenitors by fatal common envelope evolution

Cited by 19 publications

References 64 publications

Progenitors of Type IIb Supernovae. II. Observable Properties

Progenitors of Type IIb Supernovae. II. Observable Properties

Double common envelope jets supernovae (CEJSNe) by triple-star systems

The future influence of six exoplanets on the envelope properties of their parent stars on the giant branches

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