BINARY CENTRAL STARS OF PLANETARY NEBULAE DISCOVERED THROUGH PHOTOMETRIC VARIABILITY. IV. THE CENTRAL STARS OF HaTr 4 AND Hf 2-2

Hillwig, Todd C.; Bond, Howard E.; Frew, David J.; Schaub, Samuel; Bodman, Eva H. L.

doi:10.3847/0004-6256/152/2/34

Cited by 23 publications

(6 citation statements)

References 28 publications

(49 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where the emission of the shell is shown to be disrupted in several bright knots. This could be consistent with the PN being bipolar and observed nearly pole-on-such a nebular inclination would be consistent with the orbital inclination of the central binary star (Hillwig et al 2016). Nevertheless, a detailed spatio-kinematical model is needed to confirm this hypothesis, but archival VLT-UVES highresolution spatially-resolved spectroscopy (Fig.…”

Section: And [S Ii]supporting

confidence: 80%

MUSE spectroscopy of planetary nebulae with high abundance discrepancies

García‐Rojas

Morisset²,

Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present MUSE deep integral-field unit spectroscopy of three planetary nebulae (PNe) with high abundance discrepancy factors (ADF > 20): NGC 6778, M 1–42 and Hf 2–2. We have constructed flux maps for more than 40 emission lines, and use them to build extinction, electron temperature (Te), electron density (ne), and ionic abundances maps of a number of ionic species. The effects of the contribution of recombination to the auroral [N ii] and [O ii] lines on Te and the abundance maps of low-ionization species are evaluated using recombination diagnostics. As a result, low Te values and a downward gradient of Te are found toward the inner zones of each PN. Spatially, this nearly coincides with the increase of abundances of heavy elements measured using recombination lines in the inner regions of PNe, and strongly supports the presence of two distinct gas phases: a cold and metal-rich and a warm one with “normal” metal content. We have simultaneously constructed, for the first time, the ADF maps of O+ and O2 + and found that they centrally peak for all three PNe under study. We show that the main issue when trying to compute realistic abundances from either ORLs or CELs is to estimate the relative contribution of each gas component to the H i emission, and we present a method to evaluate it. It is also found that, for the studied high-ADF PNe, the amount of oxygen in the cold and warm regions is of the same order.

show abstract

Section: And [S Ii]supporting

confidence: 80%

MUSE spectroscopy of planetary nebulae with high abundance discrepancies

García‐Rojas

Morisset²,

Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Those eight are Abell63 (Bell et al 1994;Mitchell et al 2007;Afşar & Ibanoǧlu 2008), Hartl-Triton4 (Tyndall et al 2012;Hillwig et al 2016), NGC6778 (Miszalski et al 2011;Guerrero & Miranda 2012), Abell41 (Bruch et al 2001;Shimanskii et al 2008;Jones et al 2010b), Abell65 (Huckvale et al 2013;Hillwig et al 2015), Henize2-428 (Rodríguez et al 2001;Santander-García et al 2015), and the two presented here, NGC6337 (García-Díaz et al 2009) and Sp1 .…”

Section: Inclinations Of Known Pne With Binary Central Starsmentioning

confidence: 74%

“…Many of those systems were discovered through photometric variability, and while most are likely to be real binaries, additional confirmation is necessary for some of them (e.g., Kn 61; De Marco et al 2015). Along with studies confirming the binarity of several of these systems (e.g., Shimanskii et al 2008;Hillwig et al 2015Hillwig et al , 2016, discoveries of additional close binary CSPNe are helping us to better understand the nature of these systems. In addition, studies of the CS can be linked to kinematic studies of the nebulae to determine whether a causal link exists between the interaction and the nebular morphology and kinematics.…”

Section: Introductionmentioning

confidence: 99%

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

Hillwig

Jones

Marco

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…Great effort has been made to characterise the known population of binary central stars and their host nebulae. For the binary central stars, this requires simultaneous modelling of light and radial velocity curves [77,60,78]. In many cases, the intense irradiation effect leads to the production of emission lines in the 'day-side' face of the secondary; in spite of the primary being much brighter than the secondary in almost all bands, radial velocity curves of both components can be derived (the primary's from the typical absorption lines of, e.g., He II, N V and O V, and the secondary's from the emission lines C III, C IV and N III).…”

Section: Characterising the Binaries And Their Host Nebulaementioning

confidence: 99%

Binary stars as the key to understanding planetary nebulae

2017

View full text Add to dashboard Cite

Planetary nebulae are traditionally considered to represent the final evolutionary stage of all intermediate-mass stars ($\sim$0.7-8Msol). Recent evidence seems to contradict this picture. In particular, since the launch of the Hubble Space Telescope it has become clear that planetary nebulae display a wide range of striking morphologies which cannot be understood in a single star scenario, instead pointing towards a binary evolution in a majority of systems. Here, we summarise our current understanding of the importance of binarity in the formation and shaping of planetary nebulae, as well as the surprises that recent observational studies have revealed with respect to our understanding of binary evolution in general. These advances have critical implications, including for the understanding of mass transfer processes in binary stars - particularly the all-important but ever-so poorly understood `common envelope phase' - as well as the formation of cosmologically important type Ia supernovae.Comment: 20 pages, 4 figures, Review accepted for publication in Nature Astronom

show abstract

BINARY CENTRAL STARS OF PLANETARY NEBULAE DISCOVERED THROUGH PHOTOMETRIC VARIABILITY. IV. THE CENTRAL STARS OF HaTr 4 AND Hf 2-2

Cited by 23 publications

References 28 publications

MUSE spectroscopy of planetary nebulae with high abundance discrepancies

MUSE spectroscopy of planetary nebulae with high abundance discrepancies

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

Binary stars as the key to understanding planetary nebulae

Contact Info

Product

Resources

About