Grazing envelope evolution towards Type IIb supernovae

Soker, Noam

doi:10.1093/mnrasl/slx089

Cited by 22 publications

(25 citation statements)

References 60 publications

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“…The results of these runs should be taken with very great caution because mesa binary cannot properly treat the CEE. However, we do expect that in the GEE the system can get in and out of the CEE, and so the qualitative behaviour might hold, at least for the case with jets (Soker 2017).…”

Section: Numerical Limitationsmentioning

confidence: 93%

Type IIb supernovae by the grazing envelope evolution

Naiman

Sabach

Gilkis

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We simulate the evolution of binary systems with a massive primary star of 15M where we introduce an enhanced mass loss due to jets that the secondary star might launch, and find that in many cases the enhanced mass loss brings the binary system to experience the grazing envelope evolution (GEE) and form a progenitor of Type IIb supernova (SN IIb). The jets, the Roche lobe overflow (RLOF), and a final stellar wind remove most of the hydrogen-rich envelope, leaving a blue-compact SN IIb progenitor. In many cases without this jet-driven mass loss the system enters a common envelope evolution (CEE) and does not form a SN IIb progenitor. We use the stellar evolutionary code MESA binary and mimic the jet-driven mass loss with a simple prescription and some free parameters. Our results show that the jet-driven mass loss, that some systems have during the GEE, increases the parameter space for stellar binary systems to form SN IIb progenitors. We estimate that the binary evolution channel with GEE contributes about a quarter of all SNe IIb, about equal to the contribution of each of the other three channels, binary evolution without a GEE, fatal CEE (where the secondary star merges with the core of the giant primary star), and the single star channel.

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Section: Numerical Limitationsmentioning

confidence: 93%

Type IIb supernovae by the grazing envelope evolution

Naiman

Sabach

Gilkis

et al. 2019

Monthly Notices of the Royal Astronomical Society

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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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“…The existence of the above post-AGB intermediate binaries (post-AGBIBs) in the traditional orbital separation gap raises the possibility that another process plays a signifi-⋆ E-mail: kashi@ariel.ac.il † E-mail: soker@physics.technion.ac.il cant role in the evolution of post-AGBIBs. One such process to explain post-AGBIBs is the grazing envelope evolution (GEE; Soker 2017). According to the GEE, the more compact secondary star grazes the envelope of the giant star and accretes mass from its outer envelope or from its wind acceleration zone.…”

Section: Introductionmentioning

confidence: 99%

Counteracting tidal circularization with the grazing envelope evolution

Kashi

Soker

2018

Monthly Notices of the Royal Astronomical Society

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We show that substantially enhanced mass loss at periastron passages, as is expected in the grazing envelope evolution (GEE), can compensate for the circularization effect of the tidal interaction in binary systems composed of an asymptotic giant branch (AGB) star and a main sequence secondary star. By numerically integrating the equations of motion we show that under our assumptions the binary system can maintain its high eccentricity as the AGB star evolves toward the post-AGB phase. Our results can explain the high eccentricity of some post-AGB intermediate binaries (post-AGBIBs), i.e., those with an orbital periods in the range of several months to few years. In the framework of the GEE, the extra energy to sustain a high mass loss rate comes from the accretion of mass from the giant envelope or its slow wind onto a more compact secondary star. The secondary star energizes the outflow from the AGB outer envelope by launching jets from the accretion disk.

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Grazing envelope evolution towards Type IIb supernovae

Cited by 22 publications

References 60 publications

Type IIb supernovae by the grazing envelope evolution

Type IIb supernovae by the grazing envelope evolution

Progenitors of Type IIb Supernovae. II. Observable Properties

Counteracting tidal circularization with the grazing envelope evolution

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