Binary stars as the key to understanding planetary nebulae

Jones, David; Boffin, H. M. J.

doi:10.1038/s41550-017-0117

Cited by 149 publications

(108 citation statements)

References 102 publications

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“…Of the initial sample of 93 observed objects, 14 were known to host binary central stars (Jones et al 2015;Jones & Boffin 2017). Of these 14, 4 are wide binaries (orbital periods ∼ 10-1000 days) and 10 are close binaries (orbital periods ∼ 1 day).…”

Section: Planetary Nebulae With Binary Central Starsmentioning

confidence: 99%

Opening PANDORA’s box: APEX observations of CO in PNe

Guzmán-Ramírez

Gómez-Ruiz

Boffin

et al. 2018

A&A

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Context. Observations of molecular gas have played a key role in developing the current understanding of the late stages of stellar evolution. Aims. The survey Planetary nebulae AND their cO Reservoir with APEX (PANDORA) was designed to study the circumstellar shells of evolved stars with the aim to estimate their physical parameters. Methods. Millimetre carbon monoxide (CO) emission is the most useful probe of the warm molecular component ejected by low-to intermediate-mass stars. CO is the second-most abundant molecule in the Universe, and the millimetre transitions are easily excited, thus making it particularly useful to study the mass, structure, and kinematics of the molecular gas. We present a large survey of the CO (J = 3−2) line using the Atacama Pathfinder EXperiment (APEX) telescope in a sample of 93 proto-planetary nebulae and planetary nebulae. Results. CO (J = 3−2) was detected in 21 of the 93 objects. Only two objects (IRC+10216 and PN M2-9) had previous CO (J = 3−2) detections, therefore we present the first detection of CO (J = 3−2) in the following 19 objects: Frosty Conclusions. CO (J = 3−2) was detected in all 4 observed pPNe (100%), 15 of the 75 PNe (20%), one of the 4 wide binaries (25%), and in 1 of the 10 close binaries (10%). Using the CO (J = 3−2) line, we estimated the column density and mass of each source. The H 2 column density ranges from 1.7 × 10 18 to 4.2 × 10 21 cm −2 and the molecular mass ranges from 2.7 × 10 −4 to 1.7 × 10 −1 M .

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Section: Planetary Nebulae With Binary Central Starsmentioning

confidence: 99%

Opening PANDORA’s box: APEX observations of CO in PNe

Guzmán-Ramírez

Gómez-Ruiz

Boffin

et al. 2018

A&A

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“…At present, binary evolution would appear to be one of the most viable explanations for the formation of bipolar nebulae via the inevitable equatorial density enhancement (e.g., Jones & Boffin 2017). Our motivation to collect photometry measurements of the CSPN exhaustively in the UV to near-IR is also intended to establish the presence or absence of a near-IR excess, which would suggest the presence of a cooler binary companion.…”

Section: Possibility Of the Presence Of A Binary Companionmentioning

confidence: 99%

The Herschel Planetary Nebula Survey (HerPlaNS): A Comprehensive Dusty Photoionization Model of NGC6781

Otsuka

Ueta

Hoof

et al. 2017

ApJS

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We perform a comprehensive analysis of the planetary nebula (PN) NGC 6781 to investigate the physical conditions of each of its ionized, atomic, and molecular gas and dust components and the object's evolution, based on panchromatic observational data ranging from UV to radio. Empirical nebular elemental abundances, compared with theoretical predictions via nucleosynthesis models of asymptotic giant branch (AGB) stars, indicate that the progenitor is a solar-metallicity, 2.25 − 3.0 M ⊙ initial-mass star. We derive the best-fit distance of 0.46 kpc by fitting the stellar luminosity (as a function of the distance and effective temperature of the central star) with the adopted post-AGB evolutionary tracks. Our excitation energy diagram analysis indicate high excitation temperatures in the photodissociation region (PDR) beyond the ionized part of the nebula, suggesting extra heating by shock interactions between the slow AGB wind and the fast PN wind. Through iterative fitting using the Cloudy code with empirically-derived constraints, we find the best-fit dusty photoionization model of the object that would inclusively reproduce all of the adopted panchromatic observational data. The estimated total gas mass (0.41 M ⊙ ) corresponds to the mass ejected during the last AGB thermal pulse event predicted for a 2.5 M ⊙ initial-mass star. A significant fraction of the total mass (about 70 %) is found to exist in the PDR, demonstrating the critical importance of the PDR in PNe that are generally recognized as the hallmark of ionized/H

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“…As highlighted by Gianninas et al (2013), LSST could expect to find of order 100 000 white dwarfs with stellar mass companions -meaning that such systems are far from extraordinary. Furthermore, many WDMS systems will be postcommon-envelope systems (perhaps still even being surrounded by the remnant common envelope in the form of a planetary nebula; Jones & Boffin 2017;Boffin & Jones 2019) which may lead to increased local extinction as a result of dust formation in the ejected envelope (Lü et al 2013). As such, they are rather appropriate systems to constrain the importance of extinction in deriving their stellar parameters.…”

Section: Large Synoptic Survey Telescope / Vera C Rubin Observatorymentioning

confidence: 99%

Physics of Eclipsing Binaries. IV. The Impact of Interstellar Extinction on the Light Curves of Eclipsing Binaries

Jones

Conroy

Horvat

et al. 2020

ApJS

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Traditionally, the effects of interstellar extinction on binary star light curves have been treated as a uniform reduction in the observed brightness of the system that is independent of orbital phase. However, unless the orbital plane of the system coincides with the plane of the sky, or if the two stars are completely identical and present with minimal mutual irradiation and tidal/rotational distortions, then this is unlikely to be an accurate representation of the effect of interstellar extinction. Here, we present an updated treatment of interstellar extinction as incorporated in the PHOEBE 2.2 release (publicly available from http://phoebe-project.org) and assess the importance of using such an approach in the modeling of different types of binary systems. We also present the incorporation of PHOENIX model atmospheres into the PHOEBE 2.2 release, providing increased fidelity on computed observables down to lower temperatures than previously available. The importance of these new code developments is then highlighted via an extincted toy model of the eclipsing white-dwarf-subdwarf binary SDSS J235524.29+044855.7 -demonstrating that, in the age of LSST as well as complementary space-based photometric missions, a proper accounting for extinction and as well as the use of realistic model atmospheres will be essential in deriving accurate binary parameters.

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Binary stars as the key to understanding planetary nebulae

Cited by 149 publications

References 102 publications

Opening PANDORA’s box: APEX observations of CO in PNe

Opening PANDORA’s box: APEX observations of CO in PNe

The Herschel Planetary Nebula Survey (HerPlaNS): A Comprehensive Dusty Photoionization Model of NGC6781

Physics of Eclipsing Binaries. IV. The Impact of Interstellar Extinction on the Light Curves of Eclipsing Binaries

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