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

Jones, David; Boffin, H. M. J.; Rodríguez‐Gil, P.; Wesson, R.; Corradi, R. L. M.; Miszalski, B.; Mohamed, S.

doi:10.1051/0004-6361/201425454

Cited by 60 publications

(67 citation statements)

References 69 publications

(102 reference statements)

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“…We then use the difference of individual spectral lines in each spectrum from that average to create an internal wavelength calibration for the stellar spectra. Such an approach has been used successfully in the past (e.g., Jones et al 2015).…”

Section: Spectroscopymentioning

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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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: Spectroscopymentioning

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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“…while it was still on the RGB), which would not result in chemical enrichment of the secondary. However, other post-CE systems, where significant accretion from primary to secondary has occurred, indicate that the majority of the mass transfer occurs very shortly before entering the CE phase (Miszalski et al 2013;Jones et al 2015) -meaning that if there was significant transfer of non-chemically enriched material while the primary was on the RGB it is also likely that the system experienced the CE while the primary was still on the RGB. serves to show that the PN may, indeed, be the product of a CE while the primary was on the RGB.…”

Section: Discussionmentioning

confidence: 99%

On the post-common-envelope central star of the planetary nebula NGC 2346

Brown

Jones

Boffin

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The common-envelope phase is one of the most poorly understood phases of (binary) stellar evolution, in spite of its importance in the formation of a wide-range of astrophysical phenomena ranging from cataclysmic variables to cosmologically important supernova type ia, and even recently discovered gravitational wave producing black hole mergers. The central star of the planetary nebula NGC 2346 has long been held as one of the longest period post-common-envelope systems known with a published period of approximately 16 days, however the data presented were also consistent with much shorter periods of around 1 day (a more typical period among the known sample of post-common-envelope binary central stars). Here, using the modern high-stability, high-resolution spectrograph HERMES, we conclusively show the period to, indeed, be 16 days while also revising the surface gravity to a value typical of a sub-giant (rather than main-sequence) resulting in an intrinsic luminosity consistent with the recently published GAIA parallax distance. Intriguingly, the implied mass for the secondary ( 3.5 M ⊙ ) makes it, to our knowledge, the most massive post-common-envelope secondary known, whilst also indicating that the primary may be a post-RGB star.

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“…For example, the observed chemically polluted secondary star in the Necklace nebula [22]. In several other planetary nebulae (PNe), an inflated secondary main sequence (MS) star is found in a close orbit with the central star [23]. The inflation is best explained by a recent accretion phase where the accretion rate needs to be high.…”

Section: Introductionmentioning

confidence: 99%

The Morphology of the Outflow in the Grazing Envelope Evolution

Shiber

2018

Galaxies

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We study the grazing envelope evolution (GEE), where a secondary star, which orbits the surface of a giant star, accretes mass from the giant envelope and launches jets. We conduct simulations of the GEE with different half-opening angles and velocities, and simulate the onset phase and the spiralling-in phase. We discuss the resulting envelope structure and the outflow geometry. We find in the simulations of the onset phase with narrow jets that a large fraction of the ejected mass outflows along the polar directions. The mass ejected at these directions has the fastest velocity and the highest angular momentum magnitude. In the simulations of the spiralling-in phase, a large fraction of the ejected mass concentrates around the orbital plane. According to our findings, the outflow with the highest velocity is closer to the poles as we launch narrower jets. The outflow has a toroidal shape accompanied by two faster rings, one ring at each side of the equatorial plane. The interaction of the jets with the giant envelope causes these outflow structures, as we do not include in our simulations the secondary star gravity and the envelope self-gravity.

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

Cited by 60 publications

References 69 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

On the post-common-envelope central star of the planetary nebula NGC 2346

The Morphology of the Outflow in the Grazing Envelope Evolution

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