ORFEUS Observation of the Central Star of NGC 6543

Zweigle, J.; Grewing, M.; Barnstedt, J.; Gölz, M.; Gringel, W.; Haas, Christian; Hopfensitz, W.; Kappelmann, N.; Krämer, G.; Appenzeller, I.; Krautter, J.; Mandel, H.

doi:10.1007/978-94-011-5244-0_54

Cited by 3 publications

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“…The spectrum in Fig. 1 also closely matches the ORPHEUS spectrum obtained in 1993 September by Zweigle et al (1997). Note for completeness that the IUE high-resolution spectrum of NGC 6543 is dominated by saturated P Cygni profiles of C IVλλ1548.20, 1550.77 and N V λλ1238.82, 1242.80, plus well-developed blueward absorption in O V λ1371.29 and the excited line of N IV λ1718.55 (e.g.…”

Section: F U S E T I M E -S E R I E S 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: F U S E T I M E -S E R I E S 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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“…(1) Aller & Liller (1968); (2) Zweigle et al (1997); (3) Lucy & Perinotto (1987); (4) Zhekov & Perinotto (1997). Unless otherwise indicated, data are from Acker et al (1992).…”

Section: S P E C T R O S C O P I C O B S E Rvat I O N S 21 Iue Spectramentioning

confidence: 99%

The optical spectrum of the planetary nebula NGC 6543

Hyung

Aller

Feibelman

et al. 2000

Monthly Notices RAS

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A B S T R A C TWith the Hamilton echelle spectrograph at the Lick Observatory, emission-rich spectral lines of the planetary nebula NGC 6543 were secured in the wavelength range from 3550 to 10 100 A Ê . We chose two bright regions, ,8 arcsec east and ,13 arcsec north of the central star, the physical conditions and chemical abundances of which may differ as a result of the different physical characteristics involving the mass ejection of different epochs. By combining Hamilton echelle observations with archive UV data secured with the International Ultraviolet Explorer (IUE), we obtain improved diagnostics and chemical compositions for the two observed regions. The diagnostic diagram gives the average value of T e 8000 , 8300 KY and the electron number density near N e , 5000 cm 23 for most ions, while some low-excitation lines indicate much higher temperatures, i.e. T e , 10 000 KX With the construction of a photoionization model, we try to fit the observed spectra in a self-consistent way: thus, for most elements, we employ the same chemical abundances in the nebular shell; and we adopt an improved Sobolev approximation model atmosphere for the hydrogen-deficient Wolf±Rayet type central star. Within the observational errors, the chemical abundances do not seem to show any positional variation except for helium. The chemical abundances of NGC 6543 appear to be the same as in average planetary nebulae. The progenitor star may have been an object of one solar mass, most of the heavier elements of which were less plentiful than in the Sun.

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“…The interface layer in NGC 6543 can be studied using O vi emission because the physical properties of its interior hot gas have been established by Chandra observations (Chu et al 2001) and its central star is too cool to produce O vi by photoionization (T eff ∼50,000 K, Zweigle et al 1997). Far Ultraviolet Spectroscopic Explorer (FUSE ) observations of NGC 6543 have indeed detected O vi emission.…”

Section: Far Uv Observations Of Pnementioning

confidence: 99%

Planetary Nebulae and Their Central Stars in the X-ray and EUV Regions

Guerrero¹

2006

IAU

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Abstract. Einstein, EXOSAT, and ROSAT X-ray observations of planetary nebulae detected soft photospheric X-ray emission from their central stars, but the diffuse X-ray emission from the shocked fast stellar wind in their interiors could not be unambiguously resolved. The new generation of X-ray observatories, Chandra and XMM-Newton, have finally resolved the diffuse X-ray emission from shocked fast winds in planetary nebula interiors. Furthermore, these observatories have detected diffuse X-ray emission from bow-shocks of fast collimated outflows impinging on the nebular envelopes, and unexpected hard X-ray point-sources associated with the central stars of planetary nebulae. Here I review the results of these new X-ray observations of planetary nebulae and discuss the promise of future observations.

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ORFEUS Observation of the Central Star of NGC 6543

Cited by 3 publications

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Structure and clumping in the fast wind of NGC 6543

Structure and clumping in the fast wind of NGC 6543

The optical spectrum of the planetary nebula NGC 6543

Planetary Nebulae and Their Central Stars in the X-ray and EUV Regions

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