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

Hillwig, Todd C.; Jones, David; Marco, Orsola De; Bond, Howard E.; Margheim, Steve; Frew, David J.

doi:10.3847/0004-637x/832/2/125

Cited by 85 publications

(79 citation statements)

References 62 publications

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“…-The nebular waist is not coplanar with the binary plane, at odds with the results from PNe with close-binary CSs, which are found to always be coplanar (Hillwig et al 2016). -The system is a hierarchical triple where the central white dwarf forms part of a close binary, the total mass of which is 2 M .…”

Section: Update On Lotrcontrasting

confidence: 50%

“…This mass ratio effectively rules out the HB scenario, regardless of the possible mass of the hot component. However, the masses of both components can be estimated by assuming that the orbital plane lies perpendicular to the nebular symmetry axis, as predicted by PN shaping models and observed in close binary CSs Hillwig et al (2016). Ressler et al (2010) determine a nebular inclination of 59…”

Section: Analysis Of Ngc 1514mentioning

confidence: 99%

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The long-period binary central stars of the planetary nebulae NGC 1514 and LoTr 5

Jones

Winckel

Aller

et al. 2017

A&A

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The importance of long-period binaries for the formation and evolution of planetary nebulae is still rather poorly understood, which in part is due to the lack of central star systems that are known to comprise such long-period binaries. Here, we report on the latest results from the on-going Mercator-HERMES survey for variability in the central stars of planetary nebulae. We present a study of the central stars of NGC 1514, BD+30• 623, the spectrum of which shows features associated with a hot nebular progenitor as well as a possible A-type companion. Cross-correlation of high-resolution HERMES spectra against synthetic spectra shows the system to be a highly eccentric (e ∼ 0.5) double-lined binary with a period of ∼3300 days. Previous studies indicated that the cool component might be a horizontal branch star of mass ∼0.55 M , but the observed radial velocity amplitudes rule out such a low mass. If we assume that the nebular symmetry axis and binary orbital plane are perpendicular, then the data are more consistent with a post-main-sequence star ascending towards the giant branch. We also present the continued monitoring of the central star of LoTr 5, HD 112313, which has now completed one full cycle, allowing the orbital period (P∼2700 days) and eccentricity (e ∼ 0.3) to be derived. To date, the orbital periods of BD+30• 623 and HD 112313 are the longest to have been measured spectroscopically in the central stars of planetary nebulae. Furthermore, these systems, along with BD+33• 2642, comprise the only spectroscopic wide-binary central stars currently known.

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Section: Update On Lotrcontrasting

confidence: 50%

Section: Analysis Of Ngc 1514mentioning

confidence: 99%

The long-period binary central stars of the planetary nebulae NGC 1514 and LoTr 5

Jones

Winckel

Aller

et al. 2017

A&A

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“…Jones et al 2012). The extremely low probability for this perpendicularity to be a random event (Hillwig et al 2016), shows a physical link between binary stars and nebular morphology.…”

Section: Introductionmentioning

confidence: 99%

AGB winds in interacting binary stars

Bermúdez-Bustamante

Garcı́a-Segura

Steffen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We perform numerical simulations to investigate the stellar wind from interacting binary stars. Our aim is to find analytical formulae describing the outflow structure. In each binary system the more massive star is in the asymptotic giant branch and its wind is driven by a combination of pulsations in the stellar surface layers and radiation pressure on dust, while the less massive star is in the main sequence. Time averages of density and outflow velocity of the stellar wind are calculated and plotted as profiles against distance from the centre of mass and colatitude angle. We find that mass is lost mainly through the outer Lagrangian point L 2 . The resultant outflow develops into a spiral at low distances from the binary. The outflowing spiral is quickly smoothed out by shocks and becomes an excretion disk at larger distances. This leads to the formation of an outflow structure with an equatorial density excess, which is greater in binaries with smaller orbital separation. The pole-to-equator density ratio reaches a maximum value of ∼ 10 5 at Roche-Lobe Overflow state. We also find that the gas stream leaving L 2 does not form a circumbinary ring for stellar mass ratios above 0.78, when radiation pressure on dust is taken into account. Analytical formulae are obtained by curve fitting the 2-dimensional, azimuthally averaged density and outflow velocity profiles. The formulae can be used in future studies to setup the initial outflow structure in hydrodynamic simulations of common-envelope evolution and formation of planetary nebulae.

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“…These aspects include the creation of accretion driven precessing outflows or jets Miszalski et al 2013;Tocknell et al 2014 and ref. therein) and alignment of the nebula orientation with orbital inclination (Hillwig et al 2016). Low-ionisation filaments also appear to be associated with post-CE PNe (Miszalski et al 2009b;Miszalski et al 2011aMiszalski et al , 2019a, particularly in ring configurations (e.g.…”

Section: Introductionmentioning

confidence: 99%

Two’s company, three’s a crowd: SALT reveals the likely triple nature of the nucleus of the extreme abundance discrepancy factor planetary nebula Sp 3

Miszalski

Manick

Rauch³

et al. 2019

Publ. Astron. Soc. Aust.

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The substantial number of binary central stars of planetary nebulae (CSPNe) now known (∼50) has revealed a strong connection between binarity and some morphological features including jets and low-ionisation structures. However, some morphological features and asymmetries might be too complex or subtle to ascribe to binary interactions alone. In these cases a tertiary component, i.e. a triple nucleus, could be the missing ingredient required to produce these features. The only proven triple, NGC 246, is alone insufficient to investigate the shaping role of triple nuclei, but one straight-forward way to identify more triples is to search for binaries in nuclei with known visual companions. Here we demonstrate this approach with the SALT HRS discovery of a 4.81 d orbital period in the CSPN of Sp 3 which has a visual companion 0.31" away. The spectroscopic distance of the visual companion is in agreement with distance estimates to the nebula, the GAIA DR2 parallax of the central star, and the gravity distance of the central star. This supports a physical association between the visual companion and the inner 4.81 d binary, making the nucleus of Sp 3 a likely triple. We determine T eff = 68 +12 −6 kK, log g = 4.6 ± 0.2 cm s −2 and vrot = 80 ± 20 km s −1 for the primary from NLTE model atmosphere analysis. The peculiar nebula presents an apparent bipolar morphology, jets and an unexpected 'extreme' oxygen abundance discrepancy factor (adf) of 24.6 +4.1 −3.4 . The adf is inconsistent with the purported trend for longer orbital period post-CE PNe to exhibit normal adfs, further highlighting the dominant influence of selection effects in post-CE PNe. Lastly, the Type-I nebular abundances of Sp 3, whose origin is often attributed to more massive progenitors, are incongruous with the likely Galactic Thick Disk membership of Sp 3, possibly suggesting that rotation and binarity may play an important role in influencing the AGB nucleosynthesis of PNe.

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

Cited by 85 publications

References 62 publications

The long-period binary central stars of the planetary nebulae NGC 1514 and LoTr 5

The long-period binary central stars of the planetary nebulae NGC 1514 and LoTr 5

AGB winds in interacting binary stars

Two’s company, three’s a crowd: SALT reveals the likely triple nature of the nucleus of the extreme abundance discrepancy factor planetary nebula Sp 3

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