EDP Sciences
Press Release
Free Access
Issue
A&A
Volume 600, April 2017
Article Number L9
Number of page(s) 4
Section Letters
DOI https://doi.org/10.1051/0004-6361/201730700
Published online 04 April 2017

© ESO, 2017

1. Introduction

It is now clear that a binary pathway is responsible for a significant fraction of planetary nebulae (PNe), with approximately 20% of nebulae hosting detectable close-binary central stars (CSs; Miszalski et al. 2009a). Space-based observations, however, have indicated that the true close-binary fraction may, in fact, be much larger (De Marco et al. 2015). While the importance of such close binaries in forming axisymmetric PNe is now beyond question, the shaping influence of wider binaries (which avoid the common envelope phase; Ivanova et al. 2013; De Marco 2009) is still uncertain. Hydrodynamic simulations have demonstrated that the mass transfer from an asymptotic giant branch (AGB) star to a companion in a wide-binary can be, under certain circumstances, greatly enhanced with respect to the simple Bondi-Hoyle-Lyttleton accretion rate, with significant material also deposited into the orbital plane of the binary (Theuns et al. 1996). Even if the right conditions do not arise and the accretion rate onto the companion is modest, simulations show that the focussing of the AGB wind by the companion should still cause a departure from spherical symmetry (e.g. Edgar et al. 2008). The results of these simulations would seem to indicate that wide binaries can also have a significant influence on the morphology of ag="_blank">BD+33°2642B wiPB, radial rar, thcanfewd que such lonharbary" also have a ss caniat a phtml/ta aresdiffl/taondi-stiact,ectroscopir morphology ver, have laneSted Edgar et al. 24> ardaa3o. Even if tncerta, radial with lyng of ther poorlnce on the mo,ecct, be betweore cone a horizstar of BD+33°2642
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