Binary Central Stars of Planetary Nebulae

Jones, David

doi:10.3390/galaxies8020028

Cited by 10 publications

(4 citation statements)

References 84 publications

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“…Although these abundances have been revised downward [54,55], the enhanced Rb abundances combined with a lack of Zr enrichment indicate that s-process neutrons are produced by α-captures onto 22 Ne in these stars. The 22 Ne source results in higher neutron densities than the 13 C source, leading to branchings in the s-process path that preferentially The discussion in this review has thus far neglected the role of binary PN progenitor stars, but this cannot be ignored since binary interactions likely play a role in the formation and shaping of a significant fraction of PNe [e.g., [56][57][58], and can affect their chemical compositions [e.g., 59]. For sufficiently close binaries, Roche lobe overflow can lead to common envelope (CE) evolution and the truncation of the AGB [9,60].…”

Section: Discussionmentioning

confidence: 99%

Neutron-Capture Element Abundances in Planetary Nebulae

Sterling

2020

Galaxies

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Nebular spectroscopy is a valuable tool for assessing the production of heavy elements by slow neutron(n)-capture nucleosynthesis (the s-process). Several transitions of n-capture elements have been identified in planetary nebulae (PNe) in the last few years, with the aid of sensitive, high-resolution, near-infrared spectrometers. Combined with optical spectroscopy, the newly discovered near-infrared lines enable more accurate abundance determinations than previously possible, and provide access to elements that had not previously been studied in PNe or their progenitors. Neutron-capture elements have also been detected in PNe in the Sagittarius Dwarf galaxy and in the Magellanic Clouds. In this brief review, I discuss developments in observational studies of s-process enrichments in PNe, with an emphasis on the last five years, and note some open questions and preliminary trends.

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Section: Discussionmentioning

confidence: 99%

Neutron-Capture Element Abundances in Planetary Nebulae

Sterling

2020

Galaxies

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“…There are many bipolar and elliptical planetary nebulae (PNe; including some post-asymptotic giant branch nebulae) with central binary systems (e.g., Miszalski et al 2019;Orosz et al 2019;Jones 2020). The morphologies of many of these nebulae suggest that a main sequence companion accretes mass from the asymptotic giant branch (AGB) progenitor of the PN and launches jets that shape the PN (e.g., Morris 1987;Soker 1990;Sahai & Trauger 1998;Rechy-García et al 2017;Akashi & Soker 2018;Balick et al 2019;Derlopa et al 2019;Estrella-Trujillo et al 2019;Tafoya et al 2019;Balick et al 2020;Rechy-García et al 2020; for an alternative view for some bipolar PNe see, e.g., Baan et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the Nature of Jets from a Main Sequence Companion at the Onset of Common Envelope Evolution

Soker

2023

Res. Astron. Astrophys.

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I consider a flow structure by which main sequence companions that enter a common envelope evolution (CEE) with giant stars might launch jets even when the accreted gas has a sub-Keplerian specific angular momentum. I first show that after a main sequence star enters the envelope of a giant star the specific angular momentum of the accreted gas is sub-Keplerian but still sufficiently large for the accreted gas to avoid two conical-like openings along the two opposite polar directions. I suggest that the high-pressure zone that the accreted gas builds around the main sequence equatorial plane accelerates outflows along these polar opening. Most of the inflowing gas is deflected to the polar outflows, i.e., two oppositely-directed jets. The actual mass that the main sequence star accretes is only a small fraction, $\approx 0.1$, of the inflowing gas. However, the gravitational energy that this gas releases powers the inflow-outflow streaming of gas and adds energy to the common envelope ejection. This flow structure might take place during a grazing envelope evolution if it occurs, during the early CEE, and possibly in some post-CEE cases. This study increases the parameter space for main sequence stars to launch jets. Such jets might shape \add{ some morphological features in } planetary nebulae, add energy to mass removal in CEE, and power some intermediate luminosity optical transients.

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“…In this phase, mass transfer between both stars is produced either by stellar winds or by Roche-lobe overflow. According to Jones (2020) approximately 12-20 % of PNe host a post CE system, and in such systems it has been hypothesised that the ingestion of the companion can lead to the bipolar ejection of the progenitor envelope, strongly affecting the PN morphology. Other authors propose that more distant binary companions may provide an alternative mechanism for the formation of highly aspherical morphologies by influencing the direction of collimated winds from the parent star, whose axis of rotation precesses due to the influence of a companion that is not necessarily close (Garcia-Segura 1997, see discussion in Sahai & Trauger 1998).…”

Section: Introductionmentioning

confidence: 99%

Wide binaries in planetary nebulae withGaiaDR2

González-Santamaría

Manteiga

Manchado

et al. 2020

A&A

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Context. Gaia Data Release 2 (DR2) was used to select a sample of 211 central stars of planetary nebulae (CSPNe) with good quality astrometric measurements, that we refer to as GAPN, Golden Astrometry Planetary Nebulae. Gaia astrometric and photometric measurements allowed us to derive accurate distances and radii, and to calculate luminosities with the addition of self-consistent literature values. Such information was used to plot the position of these stars in a Hertzsprung-Russel (HR) diagram and to study their evolutionary status in comparison with CSPNe evolutionary tracks. Aims. The extremely precise measurement of parallaxes and proper motions in Gaia DR2 has allowed us to search for wide binary companions in a region close to each of the central stars in the GAPN sample. We are interested in establishing the presence of binary companions at large separations which could allow to add further information on the influence of binarity on the formation and evolution of planetary nebulae. We aim to study the evolutive properties of the binary pairs to check the consistency of spectral types and masses in order to better constrain the ages and evolutionary stage of the CSPNe. Methods. We limited our search to a region around 20,000 AU of each CSPN to minimise accidental detections, and only considered stars with good parallax and proper motions data, i.e. with errors below 30% in DR2. We determined that the hypothetical binary pairs should show a statistically significant agreement for the three astrometric quantities, i.e. parallax and both components of proper motions. Results. We found 8 wide binary systems among our GAPN sample. One of them is in a triple system. We compiled the astrometric and photometric measurements of these binary systems and discussed them in comparison with previously published searches for binaries in PNe. By analysing the position in the HR diagram of the companion stars using Gaia photometry, we are able to estimate their temperatures, luminosities, masses and, for one star, the evolutionary age. The derived quantities yield a consistent scenario when compared with the corresponding values as obtained for the central stars using stellar evolutionary models in the postAGB phase.

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Binary Central Stars of Planetary Nebulae

Cited by 10 publications

References 84 publications

Neutron-Capture Element Abundances in Planetary Nebulae

Neutron-Capture Element Abundances in Planetary Nebulae

On the Nature of Jets from a Main Sequence Companion at the Onset of Common Envelope Evolution

Wide binaries in planetary nebulae withGaiaDR2

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