Dynamical Simulations of the Shaping of PNe including Radiation Effects

Zweigle, J.

doi:10.1007/978-94-011-5244-0_147

Cited by 2 publications

(2 citation statements)

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“…The spectrum in Fig. 1 also closely matches the OR-PHEUS spectrum obtained in 1993 September by Zweigle et al (1997). Note for completeness that the IU E highresolution spectrum of NGC 6543 is dominated by saturated P Cygni profiles of Civλλ1548.20, 1550.77 and Nv λλ1238.82, 1242.80, plus well developed blueward absorption in Ov λ1371.29 and the excited line of Niv λ1718.55 (e.g.…”

Section: Fuse Time-series Datasupporting

confidence: 75%

Structure and clumping in the fast wind of NGC 6543

Prinja

Hodges

Massa

et al. 2007

Monthly Notices of the Royal Astronomical Society

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Far‐ultraviolet spectroscopy from the FUSE satellite is analysed to uniquely probe spatial structure and clumping in the fast wind of the central star of the H‐rich planetary nebula NGC 6543 (HD 164963). Time‐series data of the unsaturated P vλλ1118, 1128 resonance line P Cygni profiles provide a very sensitive diagnostic of variable wind conditions in the outflow. We report on the discovery of episodic and recurrent optical depth enhancements in the P v absorption troughs, with some evidence for a ∼0.17‐d modulation time‐scale. Empirical line‐synthesis modelling is used to derive physical properties, including the optical depth evolution of individual ‘events’. The characteristics of these features are essentially identical to the ‘discrete absorption components’ (DACs) commonly seen in the ultraviolet lines of massive OB stars. We have also employed the unified model atmosphere code cmfgen to explore spectroscopic signatures of clumping, and report, in particular, on the clear sensitivity of the P v lines to the clump volume filling factor. The results presented here have implications for the downward revision of mass‐loss rates in planetary nebula central stars. We conclude that the temporal structures seen in the P v lines of NGC 6543 likely have a physical origin that is similar to that operating in massive, luminous stars, and may be related to near‐surface perturbations caused by stellar pulsation and/or magnetic fields.

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Section: Fuse Time-series Datasupporting

confidence: 75%

Structure and clumping in the fast wind of NGC 6543

Prinja

Hodges

Massa

et al. 2007

Monthly Notices of the Royal Astronomical Society

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“…O vi lines in the far-UV, being strong and less affected by photoionization, are the best lines to study 10 5 K gas. High-dispersion spectroscopic observations of the O vi lines have been made with the Orbiting Retrievable Far and Extreme UV Spectrometer (ORFEUS) for only the brightest CSPNs, e.g., NGC 6543 (Zweigle et al 1997). The spectral resolution of ORF EU S, λ/∆λ = 3000, was not adequate to distinguish clearly among the interstellar and nebular O vi and H 2 absorption lines.…”

Section: Uv Views Of Hot Gas In Planetary Nebulaementioning

confidence: 99%

X-ray and UV Views of Hot Gas in Planetary Nebulae

Chu

Guerrero

Gruendl

2003

Symp. - Int. Astron. Union

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Abstract. The interior of a planetary nebula (PN) is expected to be filled with shocked fast wind from the central star. This hot gas plays the most important role in the dynamical evolution of the PN; however, its physical conditions are not well-known because useful X-ray and far-UV observations were not available until the advent of Chandra, XMMNewton, and FUSE. This paper reviews X-ray observations of the hot gas in PN interiors and far-UV observations of the interfaces between the hot gas and the dense nebular shells.

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Dynamical Simulations of the Shaping of PNe including Radiation Effects

Cited by 2 publications

References 1 publication

Structure and clumping in the fast wind of NGC 6543

Structure and clumping in the fast wind of NGC 6543

X-ray and UV Views of Hot Gas in Planetary Nebulae

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