Shaping planetary nebulae with jets in inclined triple stellar systems

Akashi, Muhammad; Soker, Noam

doi:10.1093/mnras/stx1058

Cited by 17 publications

(15 citation statements)

References 65 publications

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“…Here we differ from the work of Akashi & Soker (2017) by launching the two opposite inclined jets inside the giant envelope, and we differ from our earlier simulation by injecting inclined jets and for a long time period. As we discuss below, we might as well refer to the orbital motion of the tight binary system in the outskirts of the giant envelope as a GEE (e.g., Shiber et al 2017;Shiber 2018).…”

Section: Introductioncontrasting

confidence: 76%

“…In the present study we consider a tight binary system that enters the envelope of a giant star and experiences either a CEE or a grazing envelope evolution (GEE), or one after the other. We explore a new type of flow and base our simulation on two of our earlier studies, Akashi & Soker (2017) and Hillel et al (2017). Following a suggestion by Soker (2004), Akashi & Soker (2017) simulated the interaction of jets that a tight binary system launches into the wind of an AGB star.…”

Section: Introductionmentioning

confidence: 99%

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Inclined jets inside a common envelope of a triple stellar system

Schreier

Hillel

Soker

2019

Monthly Notices of the Royal Astronomical Society

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We conduct a three-dimensional hydrodynamical simulation to study the interaction of two opposite inclined jets inside the envelope of a giant star, and find that the jets induce many vortexes inside the envelope and that they efficiently remove mass from the envelope and form a very clumpy outflow. We assume that this very rare type of interaction occurs when a tight binary system enters the envelope of a giant star, and that the orbital plane of the tight binary system and that of the triple stellar system are inclined to each other. We further assume that one of the stars of the tight binary system accretes mass and launches two opposite jets and that the jets' axis is inclined to the angular momentum axis of the triple stellar system. The many vortexes that the jets induce along the orbit of the tight binary system inside the giant envelope might play an important role in the common envelope evolution (CEE) by distributing energy in the envelope. The density fluctuations that accompany the vortexes lead to an outflow with many clumps that might facilitate the formation of dust. This outflow lacks any clear symmetry, and it might account for very rare types of 'messy' planetary nebulae and 'messy' nebulae around massive stars. On a broader scope, our study adds to the notion that jets can play important roles in the CEE, and that they can form a rich variety of shapes of nebulae around evolved stars.

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Section: Introductioncontrasting

confidence: 76%

Section: Introductionmentioning

confidence: 99%

Inclined jets inside a common envelope of a triple stellar system

Schreier

Hillel

Soker

2019

Monthly Notices of the Royal Astronomical Society

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“…Another setting is of the tight binary system that accretes mass from the wind of the AGB star, and one or two of the stars launch jets. When the inner orbital plane of the tight binary system is inclined to the orbital plane of the tight binary system around the AGB star, the morphology of the descendant PN might be lacking any type of symmetry (Soker 2004), i.e., be a 'messy PN' (highly irregular), as demonstrated by Akashi & Soker (2017). Soker (2004) listed several PNe that might have been shaped by a triple stellar progenitor, including IC 2149, NGC 6210, and NGC 1514 that we also mention in the present study.…”

Section: Introductionmentioning

confidence: 99%

Planetary Nebulae that Cannot Be Explained by Binary Systems

Bear

Soker

2017

ApJL

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We examine the images of hundreds of planetary nebulae (PNe) and find that for about one in six PNe the morphology is too 'messy' to be accounted for by models of stellar binary interaction. We speculate that interacting triple stellar systems shaped these PNe. In this preliminary study we qualitatively classify PNe by one of four categories.(1) PNe that show no need for a tertiary star to account for their morphology. (2) PNe whose structure possesses a pronounced departure from axial-symmetry and/or mirror-symmetry. We classify these, according to our speculation, as 'having a triple stellar progenitor'. (3) PNe whose morphology possesses departure from axialsymmetry and/or mirror-symmetry, but not as pronounced as in the previous class, and are classified as 'likely shaped by triple stellar system'. (4) PNe with minor departure from axialsymmetry and/or mirror symmetry that could have been as well caused by an eccentric binary system or the inter-stellar medium. These are classified as 'maybe shaped by a triple stellar system'. Given a weight η t = 1, η l = 0.67, η m = 0.33 to classes 2, 3 and 4, respectively, we find that according to our assumption about 13 − 21% of PNe have been shaped by triple stellar systems. Although in some evolutionary scenarios not all three stars survive the evolution, we encourage the search for a triple stellar systems at the center of some PNe.

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“…Based on the nebular morphology, Bear & Soker (2017) classify Sh 2-71 as likely to have originated from a triple system, claiming that the pronounced lack of axial and/or mirror-symmetry is characteristic of such interactions. Furthermore, the hydrodynamical simulations of Akashi & Soker (2017) show that jets launched from a binary system in an inclined orbit with a tertiary AGB companion result in PN morphologies and density variations remarkably similar to those observed in Sh 2-71. This leads us to consider here the possibility that both binary A and star B form or once formed a triple system, the interacting evolution of which led to the formation of Sh 2-71.…”

Section: Introductionmentioning

confidence: 64%

“…The interactions within such a triple system as star B (the nebular progenitor in this scenario) lost its AGB envelope could feasibly have led to the formation of the unusual precessing disc found by Močnik et al (2015) in binary A. Similarly, mass transfer between star A and binary B could have led to the formation of jets (perhaps blown from the disc in binary A) which directly impacted upon the shaping of the nebula -leading to the "messy" morphology of the PN (considered to be a tell-tale sign of triple interactions; Akashi & Soker 2017;Bear & Soker 2017) as well as the observed shocks (Bohigas 2001). Furthermore, the newly identified extended emission regions, lying several arcminutes away from the centre of the PN but approximately aligned with the current positions of binary A and star B, may well be signposts of interactions within binary A or between binary A and the mass lost from star B during the PN formation episode.…”

Section: Discussionmentioning

confidence: 97%

On the triple-star origin of the planetary nebula Sh 2-71

Jones

Pejcha

Corradi

2019

Monthly Notices of the Royal Astronomical Society

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Recent studies have indicated that triple star systems may play a role in the formation of an appreciable number of planetary nebulae, however only one triple central star is known to date (and that system is likely too wide to have had much influence on the evolution of its component stars). Here, we consider the possibility that Sh 2-71 was formed by a triple system which has since broken apart. We present the discovery of two regions of emission, seemingly aligned with the proposed tertiary orbit (i.e. in line with the axis formed by the two candidate central star systems previously considered in the literature). We also perform a few simple tests of the plausibility of the triple hypothesis based on the observed properties (coordinates, radial velocities, distances and proper motions) of the stars observed close to the projected centre of the nebula, adding further support through numerical integrations of binary orbits responding to mass loss. Although a number of open questions remain, we conclude that Sh 2-71 is currently one of the best candidates for planetary nebula formation influenced by triple-star interactions.

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Shaping planetary nebulae with jets in inclined triple stellar systems

Cited by 17 publications

References 65 publications

Inclined jets inside a common envelope of a triple stellar system

Inclined jets inside a common envelope of a triple stellar system

Planetary Nebulae that Cannot Be Explained by Binary Systems

On the triple-star origin of the planetary nebula Sh 2-71

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