Binary Central Stars of Planetary Nebulae Discovered Through Photometric Variability. Iii. The Central Star of Abell 65

Hillwig, Todd C.; Frew, David J.; Louie, Melissa; Marco, Orsola De; Bond, Howard E.; Jones, David; Schaub, Samuel

doi:10.1088/0004-6256/150/1/30

Cited by 19 publications

(18 citation statements)

References 58 publications

(110 reference statements)

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“…Also visible is broad hydrogen emission similar to those seen in HFG1 (Exter et al 2005) and Abell65 (Hillwig et al 2015). In this case as well, the broad H emission with narrow absorption core corresponds to the irradiated companion.…”

Section: Spectroscopysupporting

confidence: 61%

“…Many of those systems were discovered through photometric variability, and while most are likely to be real binaries, additional confirmation is necessary for some of them (e.g., Kn 61; De Marco et al 2015). Along with studies confirming the binarity of several of these systems (e.g., Shimanskii et al 2008;Hillwig et al 2015Hillwig et al , 2016, discoveries of additional close binary CSPNe are helping us to better understand the nature of these systems. In addition, studies of the CS can be linked to kinematic studies of the nebulae to determine whether a causal link exists between the interaction and the nebular morphology and kinematics.…”

Section: Introductionmentioning

confidence: 99%

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Observational Confirmation of a Link Between Common Envelope Binary Interaction and Planetary Nebula Shaping

Hillwig

Jones

Marco

et al. 2016

ApJ

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A current issue in the study of planetary nebulae with close binary central stars is the extent to which the binaries affect the shaping of the nebulae. Recent studies have begun to show a high coincidence rate between nebulae with largescale axial or point symmetries and close binary stars. In addition, combined binary-star and spatio-kinematic modeling of the nebulae have demonstrated that all of the systems studied to date appear to have their central binary axis aligned with the primary axis of the nebula. Here we add two more systems to the list, the central stars and nebulae of NGC 6337 and Sp 1. We show both systems to be low inclination, with their binary axis nearly aligned with our line-of-sight. Their inclinations match published values for the inclinations of their surrounding nebulae. Including these two systems with the existing sample statistically demonstrates a direct link between the central binary and the nebular morphology. In addition to the systems' inclinations we give ranges for other orbital parameters from binary modeling, including updated orbital periods for the binary central stars of NGC 6337 and Sp 1.

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Section: Spectroscopysupporting

confidence: 61%

Section: Introductionmentioning

confidence: 99%

Observational Confirmation of a Link Between Common Envelope Binary Interaction and Planetary Nebula Shaping

Hillwig

Jones

Marco

et al. 2016

ApJ

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“…Binary CSPNe from the literature where parameters for both primary and secondary stars have been derived from simultaneous modelling of photometric and radial velocity observations. Hillwig et al (2015); (c) Ferguson et al (1999); (d) Hilditch et al (1996); (e) Santander-García et al (2015); (f) Hillwig et al (2010).…”

Section: Discussionmentioning

confidence: 97%

The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

Jones

Boffin

Rodríguez‐Gil

et al. 2015

A&A

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We present a study of Hen 2-155 and Hen 2-161, two planetary nebulae which bear striking morphological similarities to other planetary nebulae known to host close-binary central stars. Both central stars are revealed to be photometric variables while spectroscopic observations confirm that Hen 2-155 is host to a double-eclipsing, post-common-envelope system with an orbital period of 3 h 33 m making it one of the shortest period binary central stars known. The observations of Hen 2-161 are found to be consistent with a post-common-envelope binary of period ∼1 day. A detailed model of the central star of Hen 2-155 is produced, showing the nebular progenitor to be a hot, post-AGB remnant of approximately 0.62 M , consistent with the age of the nebula, and the secondary star to be an M dwarf whose radius is almost twice the expected zero age main sequence radius for its mass. In spite of the small numbers, all main-sequence companions, of planetary nebulae central stars, to have had their masses and radii constrained by both photometric and spectroscopic observations have also been found to display this "inflation". The cause of the "inflation" is uncertain but is probably related to rapid accretion, immediately before the recent common-envelope phase, to which the star has not yet thermally adjusted. The chemical composition of both nebulae is also analysed, showing both to display elevated abundance discrepancy factors. This strengthens the link between elevated abundance discrepancy factors and close binarity in the nebular progenitor.

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“…Single stars cannot account for many of the observed properties of elliptical and bipolar PNe (Soker 1998), and single stars cannot maintain a fast rotation over the evolution along the AGB (e.g., Soker & Harpaz 1992;Nordhaus & Blackman 2006;García-Segura et al 2014). Following earlier studies, (e.g., Bond & Livio 1990;Bond 2000), the binary shaping paradigm has gain a critical support in recent years (see reviews by Zijlstra 2015 and, in particular due to observations of many close binary systems of elliptical and bipolar PNe and a careful analysis of their morphologies, e.g., Akras et al (2015), Aller et al (2015a,b), Boffin (2015), Corradi et al (2015), , Douchin et al (2015), Fang 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), limiting the list to papers from 2015. These close binary systems went through a common envelope evolution (CEE).…”

Section: Introductionmentioning

confidence: 90%

Planetary nebula progenitors that swallow binary systems

Soker

2015

Monthly Notices of the Royal Astronomical Society

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I propose that some irregular 'messy' planetary nebulae owe their morphologies to triple-stellar evolution where tight binary systems evolve inside and/or on the outskirts the envelope of asymptotic giant branch (AGB) stars. In some cases the tight binary system can survive, in other it is destroyed. The tight binary system might breakup with one star leaving the system. In an alternative evolution, one of the stars of the brook-up tight binary system falls toward the AGB envelope with low specific angular momentum, and drowns in the envelope. In a different type of destruction process the drag inside the AGB envelope causes the tight binary system to merge. This releases gravitational energy within the AGB envelope, leading to a very asymmetrical envelope ejection, with an irregular and 'messy' planetary nebula as a descendant. The evolution of the triple-stellar system can be in a full common envelope evolution (CEE) or in a grazing envelope evolution (GEE). Both before and after destruction (if take place) the system might lunch pairs of opposite jets. One pronounced signature of triple-stellar evolution might be a large departure from axisymmetrical morphology of the descendant planetary nebula. I estimate that about one in eight non-spherical PNe is shaped by one of these triple-stellar evolutionary routes.

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Binary Central Stars of Planetary Nebulae Discovered Through Photometric Variability. Iii. The Central Star of Abell 65

Cited by 19 publications

References 58 publications

Observational Confirmation of a Link Between Common Envelope Binary Interaction and Planetary Nebula Shaping

Observational Confirmation of a Link Between Common Envelope Binary Interaction and Planetary Nebula Shaping

The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

Planetary nebula progenitors that swallow binary systems

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