The class of supernova progenitors that result from fatal common envelope evolution

Soker, Noam

doi:10.1007/s11433-019-9402-x

Cited by 14 publications

(10 citation statements)

References 114 publications

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“…Namely, the GEE might account for ≈ 0−2% of the CCSNe becoming SNe IIb. Soker (2019) estimates that the fatal CEE scenario (Lohev et al 2019) might account for 1 − 3% of all CCSNe. Recent studies suggest that single star channels also contribute to the formation of SNe IIb (e.g., Sravan et al 2018).…”

Section: Other Casesmentioning

confidence: 99%

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: Other Casesmentioning

confidence: 99%

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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“…However, they instead place extremely strong upper limits on any remaining companion and conclude that there was no stellar companion to the progenitor upon explosion (Kochanek 2018;Kerzendorf et al 2019). Most binary evolution scenarios have been ruled out because of this, and the only remaining channels are binary mergers (Nomoto et al 1995;Lohev et al 2019;Soker 2019), binary disruption after mass transfer from the secondary (Zapartas et al 2017), or the companion is a compact object. All require rather fine-tuned assumptions for the physics involved in order to produce the Cas A progenitor.…”

Section: Cassiopeia Amentioning

confidence: 99%

Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A

Hirai

Sato

Podsiadlowski

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We explore a new scenario for producing stripped-envelope supernova progenitors. In our scenario, the stripped-envelope supernova is the second supernova of the binary, in which the envelope of the secondary was removed during its red supergiant phase by the impact of the first supernova. Through 2D hydrodynamical simulations, we find that ∼50–90 % of the envelope can be unbound as long as the pre-supernova orbital separation is ≲ 5 times the stellar radius. Recombination energy plays a significant role in the unbinding, especially for relatively high mass systems (≳ 18 M⊙). We predict that more than half of the unbound mass should be distributed as a one-sided shell at about ∼10–100 pc away from the second supernova site. We discuss possible applications to known supernova remnants such as Cassiopeia A, RX J1713.7-3946, G11.2-0.3, and find promising agreements. The predicted rate is ∼0.35–1% of the core-collapse population. This new scenario could be a major channel for the subclass of stripped-envelope or type IIL supernovae that lack companion detections like Cassiopeia A.

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“…The double-degenerate model mainly involves the merger of double CO WDs (the double CO WD channel), the merger of double ONe WDs (the double ONe WD channel), and the merger of ONe WD+CO WD systems (the ONe WD+CO WD channel). In addition, an alternative way could be the merging of a WD with a core of an AGB star during the CE evolution, then in a short or a long time leading to AIC (e.g., Sabach & Soker 2014;Canals et al 2018;Soker 2019).…”

Section: The Double-degenerate Modelmentioning

confidence: 99%

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

Wang,

Liu

2020

Preprint

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The accretion-induced collapse (AIC) scenario was proposed 40 years ago as an evolutionary end state of oxygen-neon white-dwarfs (ONe WDs), linking them to the formation of neutron star (NS) systems. However, there has been no direct detection of any AIC event so far, even though there exists a lot of indirect observational evidence. Meanwhile, the binary evolutionary pathways resulting in NS formation through AIC are still not well investigated. In this article, we review recent studies on the two classic progenitor models of AIC events, i.e., the single-degenerate model (including the ONe WD+MS/RG/He star channels and the CO WD+He star channel) and the doubledegenerate model (including the double CO WD channel, the double ONe WD channel and the ONe WD+CO WD channel). Recent progress on these progenitor models is reviewed, including the binary evolutionary scenarios leading to AIC events, the initial parameter space for producing AIC events, and the related objects (e.g., the pre-AIC systems and the post-AIC systems). For the single-degenerate model, the pre-AIC systems (i.e., the progenitor systems of AIC events) could potentially be identified as cataclysmic variables (such as classical novae, recurrent novae, Ne novae and He novae), symbiotics and supersoft X-ray sources in the observations, whereas the post-AIC systems (i.e., NS systems) could potentially be identified as low-/intermediate-mass X-ray binaries, and the resulting low-/intermediate-mass binary pulsars, most notably millisecond pulsars. For the double-degenerate model, the pre-AIC systems are close double WDs with short orbital periods, whereas the post-AIC systems are single isolated NSs that may correspond to a specific kind of NS with peculiar properties. We also review the predicted rates of AIC events, the mass distribution of NSs produced via AIC, and the gravitational wave (GW) signals from double WDs that are potential GW sources in the Galaxy in the context of future space-based GW detectors, such as LISA, TianQin and Taiji, etc. Recent theoretical and observational constraints on the detection of AIC events are summarized. In order to confirm the existence of the AIC process, and resolve this long-term issue presented by current stellar evolution theories, more numerical simulations and observational identifications are required.

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The class of supernova progenitors that result from fatal common envelope evolution

Cited by 14 publications

References 114 publications

Type IIb supernovae by the grazing envelope evolution

Type IIb supernovae by the grazing envelope evolution

Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

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