Planetary Nebulae: What Can They Tell Us About Close Binary Evolution?

Jones, David

doi:10.1051/eas/1571023

Cited by 7 publications

(5 citation statements)

References 16 publications

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“…The notion that binary stellar systems (e.g, Bond & Livio 1990;Bond 2000;Zijlstra 2015) or planetary systems (e.g, De Marco & Soker 2011) shape planetary nebulae (PNe) has gained a huge support over the years, both from theoretical considerations that point to the difficulties of models based on single asymptotic giant branch (AGB) stellar progenitors to shape PNe (e.g., Soker & Harpaz 1992;Nordhaus & Blackman 2006;García-Segura et al 2014), and from a large number of observations and their analysis (e.g., from 2015 on, Akras et al 2015;Aller et al 2015a,b;Boffin 2015;Corradi et al 2015;Decin et al 2015;Douchin et al 2015;Fang et al 2015;Gorlova et al 2015;Hillwig et al 2015;Jones 2015;Jones et al 2015;Martínez González et al 2015;Miszalski et al 2015;Močnik et al 2015;Montez et al 2015;Jones et al 2016;Chiotellis et al 2016;Akras et al 2016;García-Rojas et al 2016;Jones 2016;Hillwig et al 2016a,b;Bond et al 2016;Chen et al 2016;Madappatt et al 2016;Ali et al 2016;Hillwig et al 2017). In most cases of shaping by binary interaction, jets are involved (e.g., Morris 1987;Soker 1990;Sahai & Trauger 1998;Boffin et al 2012;Huarte-Espinosa et al...…”

Section: Introductionmentioning

confidence: 99%

Shaping planetary nebulae with jets in inclined triple stellar systems

Akashi¹,

Soker²

2017

Monthly Notices of the Royal Astronomical Society

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We conduct three-dimensional hydrodynamical simulations of two opposite jets launched obliquely to the orbital plane around an asymptotic giant branch (AGB) star and within its dense wind, and demonstrate the formation of a 'messy' planetary nebula (PN), namely, a PN lacking any type of symmetry (highly irregular). In building the initial conditions we assume that a tight binary system orbits the AGB star, and that the orbital plane of the tight binary system is inclined to the orbital plane of the binary system and the AGB star (the triple system plane). We further assume that the accreted mass on to the tight binary system forms an accretion disk around one of the stars, and that the plane of the disk is tilted to the orbital plane of the triple system. The highly asymmetrical and filamentary structures that we obtain support the notion that messy PNe might be shaped by triple stellar systems.

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Section: Introductionmentioning

confidence: 99%

Shaping planetary nebulae with jets in inclined triple stellar systems

Akashi¹,

Soker²

2017

Monthly Notices of the Royal Astronomical Society

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“…† E-mail: brent@saao.ac.za because of new theoretical advances complemented by direct and growing evidence for binarity in PNe . Almost 50 close binaries are now known, with the majority exhibiting orbital periods of 1 d or less (Miszalski et al 2011a;Jones 2015). The short orbital periods are the result of at least one common-envelope (CE) phase (Paczynski 1976;Ivanova et al 2013) and together they represent the youngest accessible window into the aftermath of this critical and unobserved phase of binary stellar evolution.…”

Section: Introductionmentioning

confidence: 99%

SALT HRS discovery of a long-period double-degenerate binary in the planetary nebula NGC 1360

Miszalski

Manick

Mikołajewska

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Whether planetary nebulae (PNe) are predominantly the product of binary stellar evolution as some population synthesis models (PSM) suggest remains an open question. Around 50 short period binary central stars (P ∼ 1 d) are known, but with only four with measured orbital periods over 10 d, our knowledge is severely incomplete. Here we report on the first discovery from a systematic SALT HRS survey for long period binary central stars. We find a 142 d orbital period from radial velocities of the central star of NGC 1360, HIP 16566. NGC 1360 appears to be the product of common-envelope (CE) evolution, with nebula features similar to post-CE PNe, albeit with an orbital period considerably longer than expected to be typical of post-CE PSM. The most striking feature is a newly-identified ring of candidate low-ionisation structures (LIS). Previous spatio-kinematic modelling of the nebula gives a nebula inclination of 30 ± 10 deg, and assuming the binary nucleus is coplanar with the nebula, multi-wavelength observations best fit a more massive, evolved WD companion. A WD companion in a 142 d orbit is not the focus of many PSM, making NGC 1360 a valuable system with which to improve future PSM work. HIP 16566 is amongst many central stars in which large radial velocity variability was found by low-resolution surveys. The discovery of its binary nature may indicate long period binaries may be more common than PSM models predict.

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“…If the formation and shaping of most PNe is a result of binary evolution (e.g., see review [12]), then the majority of CSPNe should have binary companions. Searches for such companions have been made using photometric (and radial velocity) variability over many decades starting with the early work by [19] that revealed companions in 10-15% of a sample of ∼100 CSPNe with periods, P < ∼ 3 d. Recent searches have now considerably increased the sample size-with a dearth of objects at long periods (P > 3 d, [20][21][22]). The small period (thus small orbital separation) of the binaries suggests that these objects must have undergone common-envelope (CE) evolution at an earlier phase of their evolution.…”

Section: Binary Companions and Disks In Post-agb And Post-rgb Objectsmentioning

confidence: 99%

Observing Planetary and Pre-Planetary Nebulae with the James Webb Space Telescope

Sahai

2020

Galaxies

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Most stars in the Universe that leave the main sequence in a Hubble time will end their lives evolving through the Planetary Nebula (PN) evolutionary phase. The heavy mass loss which occurs during the preceding Asymptotic Giant Branch (AGB) phase is important across astrophysics, dramatically changing the course of stellar evolution, contributing to the dust content of the interstellar medium, and influencing its chemical composition. The evolution from the AGB phase to the PN phases remains poorly understood, especially the dramatic transformation that occurs in the morphology of the mass-ejecta as AGB stars enter the post-AGB phase and their round circumstellar envelopes evolve into pre-PNe (PPNe) and then to PNe. The majority of PPNe and PNe deviate strongly from spherical symmetry. Strong binary interactions most likely play a fundamental role in influencing this evolutionary phase, but the details of these interactions remain shrouded in mystery. Thus, understanding the formation and evolution of these objects is of wide astrophysical importance. PNe have long been known to emit across a very large span of wavelengths, from the radio to X-rays. Extensive use of space-based observatories at X-ray (Chandra/ XMM-Newton), optical (HST) and mid- to far-infrared (Spitzer, Herschel) wavelengths in recent years has produced significant new advances in our knowledge of these objects. Given the expected advent of the James Webb Space Telescope (JWST) in the near future, we focus on future high-angular-resolution, high-sensitivity observations at near and mid-IR wavelengths with JWST that can help in addressing the major unsolved problems in the study of PNe and their progenitors.

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Planetary Nebulae: What Can They Tell Us About Close Binary Evolution?

Cited by 7 publications

References 16 publications

Shaping planetary nebulae with jets in inclined triple stellar systems

Shaping planetary nebulae with jets in inclined triple stellar systems

SALT HRS discovery of a long-period double-degenerate binary in the planetary nebula NGC 1360

Observing Planetary and Pre-Planetary Nebulae with the James Webb Space Telescope

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