Simulating the onset of grazing envelope evolution of binary stars

Shiber, Sagiv; Kashi, Amit; Soker, Noam

doi:10.1093/mnrasl/slw208

Cited by 56 publications

(62 citation statements)

References 36 publications

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“…In planetary nebulae the jets might be formed before or after the main nebular shell (e.g., Tocknell et al 2014). In those planetary nebulae with ears similar to those of SNRs, it is possible that the age of the jets and nebular shells is similar, and the jets have played a role in ejecting the nebula, possibly in a feedback process (e.g., Shiber et al 2017). We hence speculate that the formation processes of ears in planetary nebulae might have some similarity to the formation of ears in CCSNRs, and in any case, both processes involve energetic jets.…”

Section: Discussion and Summarymentioning

confidence: 99%

Core collapse supernova remnants with ears

Grichener¹,

Soker²

2017

Monthly Notices of the Royal Astronomical Society

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We study the morphologies of core collapse supernova remnants (CCSNRs) and find that about third of CCSNRs in our sample have two opposite 'ears' protruding from their main shell. We assume that the ears are formed by jets, and argue that these properties are compatible with the expectation from the explosion jet feedback mechanism (JFM). Based on previous studies of ears in CCSNRs and the similarity of some ears to those found in planetary nebulae, we assume that the ears are inflated by jets that are launched during the explosion, or a short time after it. Under simple geometrical assumptions we find that the extra kinetic energy of the ears is in the range of 1 to 10 percents of the explosion energy. As not all of the kinetic energy of the jets ends in the ears, we estimate that the typical kinetic energy in the jets that inflated the ears, under our assumptions, is about 5 to 15 percents of the explosion energy. This study supports a serious consideration of jet-driven core-collapse supernova mechanisms.

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Section: Discussion and Summarymentioning

confidence: 99%

Core collapse supernova remnants with ears

Grichener¹,

Soker²

2017

Monthly Notices of the Royal Astronomical Society

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“…This particle is the companion star. We launch jets in the same manner as in Shiber et al (2017) and Shiber, & Soker (2018). The salient points are as follows.…”

Section: Numerical Set-upmentioning

confidence: 99%

“…Armitage & Livio (2000) and Chevalier (2012) examined the ejection of the CE by jets launched from a NS that inspirals inside the giant envelope. Later studies follow this idea while considering different companions (e.g., Soker 2004;Papish et al 2015;Soker 2015Soker , 2016aMoreno Méndez et al 2017;Shiber et al 2017;Shiber, & Soker 2018;López-Cámara et al 2019).…”

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confidence: 99%

Companion-launched jets and their effect on the dynamics of common envelope interaction simulations

Shiber

Iaconi

Marco

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We conduct three-dimensional hydrodynamic simulations of the common envelope binary interaction and show that if the companion were to launch jets while interacting with the giant primary star's envelope, the jets would remove a substantial fraction of the envelope's gas. We use the setup and numerical code of an earlier common envelope study that did not include jets, with a 0.88-M , 83-R red giant star and a 0.3-M companion. The assumption is that the companion star accretes mass via an accretion disk that is responsible for launching the jets which, in the simulations, are injected numerically. For the first time we conduct simulations that include jets as well as the gravitational energy released by the inspiraling core-companion system. We find that simulations with jets unbind approximately three times as much envelope mass than identical simulations that do not include jets, though the total fraction of unbound gas remains below 50% for these particular simulations. The jets generate high velocity outflows in the polar directions. The jets also increase the final corecompanion orbital separation and lead to a kick velocity of the core-companion binary system. Our results show that, if able to form, jets could play a crucial role in ejecting the envelope and in shaping the outflow.

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“…The interaction of the jets with the outskirts of the envelope of the giant star leads to a complicated flow structure (e.g., Shiber et al (2017)). In this phase the jets mostly interact with the envelope outskirts and with the dense base of the wind, and do not expand to large distances (section 3).…”

Section: Shaping the Outflowmentioning

confidence: 99%

Shaping Planetary Nebulae with Jets and the Grazing Envelope Evolution

Soker

2020

Galaxies

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I argue that the high percentage of PNe that are shaped by jets show that main sequence stars in binary systems can accrete mass at a high rate from an accretion disk and launch jets. Not only this allows jets to shape PNe, but this also points to the importance of jets in other types of binary systems and in other processes. These processes include the grazing envelope evolution (GEE), the common envelope evolution (CEE), and the efficient conversion of kinetic energy to radiation in outflows. As well, the jets point to the possibility that many systems launch jets as they enter the CEE, possibly through a GEE phase. The other binary systems where jets might play significant roles include intermediate-luminosity optical transients (ILOTs), supernova impostors (including pre-explosion outbursts), post-CEE binary systems, post-GEE binary systems, and progenitors of neutron star binary systems and black hole binary systems. One of the immediate consequences is that the outflow of these systems is highly-non-spherical, including bipolar lobes, jets, and rings.

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Simulating the onset of grazing envelope evolution of binary stars

Cited by 56 publications

References 36 publications

Core collapse supernova remnants with ears

Core collapse supernova remnants with ears

Companion-launched jets and their effect on the dynamics of common envelope interaction simulations

Shaping Planetary Nebulae with Jets and the Grazing Envelope Evolution

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