The High‐Excitation Planetary Nebula NGC 246: Optical and Near‐Ultraviolet Observations and Two‐dimensional Numerical Models

Szentgyorgyi, Andrew; Raymond, J. C.; Franco, J.; Villaver, E.; López‐Martín, L.

doi:10.1086/377123

Cited by 14 publications

(19 citation statements)

References 58 publications

(61 reference statements)

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“…4(a) for path 2 over this area. However, the appearance of this ‘hole’ is very similar to that in the image of the high‐excitation PN NGC 246 presented by Szentgyorgyi et al (2003); a common explanation is suggested.…”

Section: Discussionsupporting

confidence: 64%

The bipolarity of the highest Galactic latitude planetary nebula, LoTr 5 (PN G339.9+88.4), around IN Com

Graham

Meaburn

López³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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High‐resolution, spatially resolved, long‐slit profiles of the [O iii] 5007‐Å emission line of the highest Galactic latitude planetary nebula, LoTr 5, have been obtained with the Manchester Echelle Spectrometer (MES‐SPM) on the San Pedro Martir (SPM) 2.1‐m telescope. These are compared with a deep narrow‐band [O iii] 5007‐Å mosaic image obtained with the same system. This faint nebula, at a distance of ≥500 pc from the Galactic plane, is found to be expanding asymmetrically. Some form of bipolar structure is suggested by modelling the position–velocity arrays of line profiles and the new [O iii] 5007‐Å image. Interestingly, the modelled bipolar axis is nearly perpendicular to the orbital plane of the IN Com binary system; this supports the theories which predict that binary systems play a part in shaping the outflow. Evidence for interaction of the envelope of LoTr 5 with its local interstellar medium is also considered.

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Section: Discussionsupporting

confidence: 64%

The bipolarity of the highest Galactic latitude planetary nebula, LoTr 5 (PN G339.9+88.4), around IN Com

Graham

Meaburn

López³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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“…The western edge is considerably brighter than the rest of the shell. This, and the displacement of the PN nucleus from the geometrical center of the nebula support the idea of the interaction with the ISM (for more details see, e.g., Muthu et al 2000;Szentgyorgyi et al 2003). The central star of this PN (HIP 3678) is a known hierarchical triple stellar system with an early to mid-K dwarf (K2-K5, named HIP 3678 B) and a mid M dwarf (M5-M6, named HIP 3678 C) as companions of the primary white dwarf (see Adam & Mugrauer 2014).…”

Section: Ngc 246supporting

confidence: 73%

Planetary nebulae seen with TESS: Discovery of new binary central star candidates from Cycle 1

Aller

Lillo-Box

Jones

et al. 2020

A&A

192

110

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Context. It is now clear that binarity plays a crucial role in many aspects of planetary nebulae (PNe), particularly the striking morphologies that they show. To date, there are ∼ 60 bCSPNe known. However, both theory and observation indicates that this represents only the tip of the iceberg, with the Galactic PN population hosting orders of magnitude more. Aims. We are involved in a search for new bCSPNe to enhance the statistical validation of the key role of binarity in the formation and shaping of PNe. New discoveries of bCSPNe and their characterization have important implications not only in understanding PN evolution but also in understanding binary evolution and the poorly-understood common-envelope phase. Methods. We used data from the TESS satellite to search for variability in the eight CSPNe that belong to the two-minute cadence preselected targets in Cycle 1, which have available pipeline-extracted light curves. We identified strong periodicities and analysed them in the context of the binary scenario. Results. All the CSPNe but one (Abell 15) show clear signs of periodic variability in TESS. The cause of this variability can be attributed to different effects, some of them requiring the presence of a companion star. We find simple sinusoidal modulations in several of the systems, compatible to irradiation effects. In addition, two of the central stars (PG 1034+001 and NGC 5189) also show photometric variations due to ellipsoidal variations and other signs of variability probably caused by star spots and/or relativistic Doppler-beaming. Especially interesting is the case of the well-studied Helix Nebula, in which we constructed a series of binary models to explain the modulations we see in the light curve. We find that the variability constrains the possible companion to be very low-mass main-sequence star or sub-stellar object. We also identify with a great detail the individual pulsation frequencies of NGC 246.

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“…We find that the vortices will affect almost all bow shock structures and PNe will interact with them at some point during their evolution. A higher speed case carried out by VGM also revealed similar structures forming in the AGB wind bow shock (Szentgyorgyi et al 2003).…”

Section: Resultsmentioning

confidence: 71%

The interaction of planetary nebulae and their asymptotic giant branch progenitors with the interstellar medium

Wareing¹,

Zijlstra²,

O’Brien³

2007

Monthly Notices of the Royal Astronomical Society

111

132

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Interaction with the interstellar medium (ISM) cannot be ignored in understanding planetary nebula (PN) evolution and shaping. In an effort to understand the range of shapes observed in the outer envelopes of PNe, we have run a comprehensive set of three‐dimensional hydrodynamic simulations, from the beginning of the asymptotic giant branch (AGB) superwind phase until the end of the post‐AGB/PN phase. A ‘triple‐wind’ model is used, including a slow AGB wind, fast post‐AGB wind and third wind reflecting the linear movement through the ISM. A wide range of stellar velocities, mass‐loss rates and ISM densities have been considered. We find that ISM interaction strongly affects outer PN structures, with the dominant shaping occurring during the AGB phase. The simulations predict four stages of PN–ISM interaction whereby (i) the PN is initially unaffected, (ii) then limb‐brightened in the direction of motion, (iii) then distorted with the star moving away from the geometric centre, and (iv) finally so distorted that the object is no longer recognizable as a PN and may not be classed as such. Parsec‐size shells around PNe are predicted to be common. The structure and brightness of ancient PNe are largely determined by the ISM interaction, caused by rebrightening during the second stage; this effect may address the current discrepancies in Galactic PN abundance. The majority of PNe will have tail structures. Evidence for strong interaction is found for all known PNe in globular clusters.

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The High‐Excitation Planetary Nebula NGC 246: Optical and Near‐Ultraviolet Observations and Two‐dimensional Numerical Models

Cited by 14 publications

References 58 publications

The bipolarity of the highest Galactic latitude planetary nebula, LoTr 5 (PN G339.9+88.4), around IN Com

The bipolarity of the highest Galactic latitude planetary nebula, LoTr 5 (PN G339.9+88.4), around IN Com

Planetary nebulae seen with TESS: Discovery of new binary central star candidates from Cycle 1

The interaction of planetary nebulae and their asymptotic giant branch progenitors with the interstellar medium

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