UV spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae: NGC 2867, NGC 5189, NGC 6905, Pb 6 and Sand 3

Keller, Graziela R.; Bianchi, Luciana; Maciel, W. J.

doi:10.1093/mnras/stu878

Cited by 18 publications

(27 citation statements)

References 41 publications

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“…Unfortunately, since then no efforts have been made in the literature to determine if NGC 5189 has a close binary nucleus. The central star has a [WO1] spectral type (Crowther et al 1998) and is amongst the hottest of all central stars at 165 18 −8 kK (Keller et al 2014). Ciardullo & Bond (1996) monitored the central star for ∼9 hours and found a low-amplitude pulsation period of 11.51 ± 0.05 min that is typical of stars of its ilk (Ciardullo & Bond 1996;Gonzalez-Perez et al 1996), but noted no other variability that might otherwise indicate a companion is present.…”

Section: Sample Selectionmentioning

confidence: 97%

“…Table 6 lists companion masses m2 calculated for a range of inclination values and an adopted m1 mass of 0.596 M⊙ for the [WO1] primary. The value of m1 was calculated as an average of the masses of Miller Bertolami & Althaus ( 2006) evolutionary tracks either side of the location of NGC 5189 in figure 13 of Keller et al (2014). There are several caveats associated with this assumption.…”

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

“…Firstly, the mass estimates derived from interpolating between evolutionary tracks are distance dependent and distances to PNe are notoriously uncertain. Keller et al (2014) adopted a distance of 0.55 kpc to NGC 5189 (Stanghellini et al 2008), but the distance may be as large as 1.44 ± 0.27 kpc based on extinction and kinematic distance estimates (Frew 2008). The luminosity would therefore increase from ∼ 2.73 L⊙ (Keller et al 2014) to ∼ 3.86 L⊙ (Frew 2008), resulting in a mass closer to ∼0.62 M⊙.…”

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

“…Keller et al (2014) adopted a distance of 0.55 kpc to NGC 5189 (Stanghellini et al 2008), but the distance may be as large as 1.44 ± 0.27 kpc based on extinction and kinematic distance estimates (Frew 2008). The luminosity would therefore increase from ∼ 2.73 L⊙ (Keller et al 2014) to ∼ 3.86 L⊙ (Frew 2008), resulting in a mass closer to ∼0.62 M⊙. However, it is not necessarily a matter of adopting this mass as this method of estimating CSPNe masses does not agree well with spectroscopic mass estimates for CSPNe (see section 4.2.3 of Moe & De Marco 2006 and ref.…”

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

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A radial velocity survey for post-common-envelope Wolf–Rayet central stars of planetary nebulae: first results and discovery of the close binary nucleus of NGC 5189★

Manick

Miszalski

McBride

2015

Monthly Notices of the Royal Astronomical Society

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The formation of Wolf-Rayet central stars of planetary nebulae ([WR] CSPNe) whose spectroscopic appearance mimics massive WR stars remains poorly understood. Least understood is the nature and frequency of binary companions to [WR] CSPNe that may explain their H-deficiency. We have conducted a systematic radial velocity (RV) study of 6 [WR] CSPNe to search for post-common-envelope (post-CE) [WR] binaries. We used a cross-correlation method to construct the RV time-series as successfully done for massive close binary WR stars. No significant RV variability was detected for the late-[WC] type nuclei of Hen 2-113, Hen 3-1333, PMR 2 and Hen 2-99. Significant, large-amplitude variability was found in the [WC4] nucleus of NGC 5315. In the [WO1] nucleus of NGC 5189 we discovered significant periodic variability that reveals a close binary with P orb = 4.04 ± 0.1 d. We measured a semi-amplitude of 62.3 ± 1.3 km s −1 that gives a companion mass of m 2 0.5 M ⊙ or m 2 = 0.84 M ⊙ (assuming i = 45 • ). The most plausible companion type is a massive WD as found in Fleming 1. The spectacular nebular morphology of NGC 5189 fits the pattern of recently discovered post-CE PNe extremely well with its dominant low-ionisation structures (e.g. as in NGC 6326) and collimated outflows (e.g. as in Fleming 1). The anomalously long 4.04 d orbital period is either a once-off (e.g. NGC 2346) or it may indicate there is a sizeable population of [WR] binaries with massive WD companions in relatively wide orbits, perhaps influenced by interactions with the strong [WR] wind.

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Section: Sample Selectionmentioning

confidence: 97%

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

Section: Orbital Period Analysis and Mass Functionmentioning

confidence: 99%

See 2 more Smart Citations

A radial velocity survey for post-common-envelope Wolf–Rayet central stars of planetary nebulae: first results and discovery of the close binary nucleus of NGC 5189★

Manick

Miszalski

McBride

2015

Monthly Notices of the Royal Astronomical Society

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“…0.04 (in one case even > 0.04). The recent study of five very hot hydrogen-deficient central stars by Keller et al (2014) indicates similar neon mass fractions: 0.01. . .…”

Section: Discussionmentioning

confidence: 82%

Hot bubbles of planetary nebulae with hydrogen-deficient winds - II. Analytical approximations with application to BD+30$^\circ$3639

Heller,

Jacob,

Schönberner

et al. 2018

Preprint

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Context. The first high-resolution X-ray spectroscopy of a planetary nebula, BD +30 • 3639, opened the possibility to study plasma conditions and chemical compositions of X-ray emitting "hot" bubbles of planetary nebulae in much greater detail than before. Aims. We investigate (i) how diagnostic line ratios are influenced by the bubble's thermal structure and chemical profile, (ii) whether the chemical composition inside the bubble of BD +30 • 3639 is consistent with the hydrogen-poor composition of the stellar photosphere/wind, and (iii) whether hydrogen-rich nebular matter has already been added to the bubble of BD +30 • 3639 by evaporation. Methods. We applied an analytical, 1-D model for wind-blown bubbles with temperature and density profiles based on self-similar solutions including thermal conduction. We constructed also heat-conduction bubbles with a chemical stratification. The X-ray emission is computed using the well-documented CHIANTI code. These bubble models are used to re-analyse the high-resolution X-ray spectrum from the hot bubble of BD +30 • 3639. Results. We found that our 1-D heat-conducting bubble models reproduce the observed line ratios much better than plasmas with single electron temperatures. In particular, all the temperature-and abundance-sensitive line ratios are consistent with BD +30 • 3639 X-ray observations for (i) an intervening column density of neutral hydrogen, N H = 0.20 +0.05 −0.10 ×10 22 cm −2 , (ii) a characteristic bubble X-ray temperature of T X = 1.8 ± 0.1 MK together with (iii) a very high neon mass fraction of about 0.05, virtually as high as that of oxygen. For lower values of N H , it cannot be excluded that the hot bubble of BD +30 • 3639 contains a small amount of "evaporated" (or mixed) hydrogen-rich nebular matter. Given the possible range of N H , the fraction of evaporated hydrogen-rich matter cannot exceed 3 % of the bubble mass. Conclusions. The diffuse X-ray emission from BD +30 • 3639 can well be explained by models of wind-blown bubbles with thermal conduction and a chemical composition equal to that of the hydrogen-poor and carbon-, oxygen-, and neon-rich stellar surface.

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Hot bubbles of planetary nebulae with hydrogen-deficient winds

Heller

Jacob

Schönberner

et al. 2018

A&A

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Context. The first high-resolution X-ray spectroscopy of a planetary nebula, BD +30 • 3639, opened the possibility to study plasma conditions and chemical compositions of X-ray emitting "hot" bubbles of planetary nebulae in much greater detail than before. Aims. We investigate (i) how diagnostic line ratios are influenced by the bubble's thermal structure and chemical profile, (ii) whether the chemical composition inside the bubble of BD +30 • 3639 is consistent with the hydrogen-poor composition of the stellar photosphere and wind, and (iii) whether hydrogen-rich nebular matter has already been added to the bubble of BD +30 • 3639 by evaporation. Methods. We applied an analytical, one-dimensional (1D) model for wind-blown bubbles with temperature and density profiles based on self-similar solutions including thermal conduction. We also constructed heat-conduction bubbles with a chemical stratification. The X-ray emission was computed using the well-documented CHIANTI code. These bubble models are used to re-analyse the high-resolution X-ray spectrum from the hot bubble of BD +30 • 3639. Results. We found that our 1D heat-conducting bubble models reproduce the observed line ratios much better than plasmas with single electron temperatures. In particular, all the temperature-and abundance-sensitive line ratios are consistent with BD +30 • 3639 X-ray observations for (i) an intervening column density of neutral hydrogen, N H = 0.20 +0.05 −0.10 ×10 22 cm −2 , (ii) a characteristic bubble X-ray temperature of T X = 1.8 ± 0.1 MK together with (iii) a very high neon mass fraction of about 0.05, virtually as high as that of oxygen. For lower values of N H , we cannot exclude the possibility that the hot bubble of BD +30 • 3639 contains a small amount of "evaporated" (or mixed) hydrogen-rich nebular matter. Given the possible range of N H , the fraction of evaporated hydrogen-rich matter cannot exceed 3% of the bubble mass. Conclusions. The diffuse X-ray emission from BD +30 • 3639 can be well explained by models of wind-blown bubbles with thermal conduction and a chemical composition equal to that of the hydrogen-poor and carbon-, oxygen-, and neon-rich stellar surface.Article published by EDP Sciences A98, page 1 of 23 A&A 620, A98 (2018)

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UV spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae: NGC 2867, NGC 5189, NGC 6905, Pb 6 and Sand 3

Cited by 18 publications

References 41 publications

A radial velocity survey for post-common-envelope Wolf–Rayet central stars of planetary nebulae: first results and discovery of the close binary nucleus of NGC 5189★

A radial velocity survey for post-common-envelope Wolf–Rayet central stars of planetary nebulae: first results and discovery of the close binary nucleus of NGC 5189★

Hot bubbles of planetary nebulae with hydrogen-deficient winds - II. Analytical approximations with application to BD+30$^\circ$3639

Hot bubbles of planetary nebulae with hydrogen-deficient winds

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