The Spectrum of NGC 6543 and its Nucleus.

Swings, Polydore

doi:10.1086/144218

Cited by 5 publications

(2 citation statements)

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“…The central star within the second-brightest diffuse X-ray PN, NGC 6543, also has long been classified as Wolf-Rayet type (Swings 1940). Its wind speed and mass loss rate (1750 km s −1 and ∼ 10 −7…”

Section: Indeed Among the Prototype [Wcl] Objects Is Bd +30mentioning

confidence: 99%

“…Indeed, among the prototype [WCL] objects is BD +30 • 3639, the first well-established -and brightest -example of diffuse X-ray emission from a PN (Kreysing et al 1992;Kastner et al 2000Kastner et al , 2002. The central star within the second-brightest diffuse X-ray PN, NGC 6543, also has long been classified as Wolf-Rayet type (Swings 1940). Its wind speed and mass loss rate (1750 km s −1 and ∼ 10 −7 M ⊙ yr −1 , respectively; Perinotto et al (1989)) are quite large, explaining the star's broad emission line spectrum.…”

Section: Introductionmentioning

confidence: 99%

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X‐Ray Imaging of Planetary Nebulae with Wolf‐Rayet–type Central Stars: Detection of the Hot Bubble in NGC 40

Montez

Kastner

Marco

et al. 2005

ApJ

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We present the results of Chandra X-ray Observatory (CXO) observations of the planetary nebulae (PNs) NGC 40 and Hen 2-99. Both PNs feature late-type Wolf-Rayet central stars that are presently driving fast (∼ 1000 km s −1 ), massive winds into denser, slow-moving (∼10 km s −1 ) material ejected during recently terminated asymptotic giant branch (AGB) evolutionary phases. Hence, these observations provide key tests of models of wind-wind interactions in PNs. In NGC 40, we detect faint, diffuse X-ray emission distributed within a partial annulus that lies nested within a ∼ 40 ′′ diameter ring of nebulosity observed in optical and near-infrared images. Hen 2-99 is undetected. The inferred X-ray temperature (T X ∼ 10 6 K) and luminosity (L X ∼ 2 × 10 30 ergs s −1 ) of NGC 40 are the lowest measured thus far for any PN displaying diffuse X-ray emission. These results, combined with the ring-like morphology of the X-ray emission -2 -from NGC 40, suggest that its X-ray emission arises from a "hot bubble" that is highly evolved and is generated by a shocked, quasi-spherical fast wind from the central star, as opposed to AGB or post-AGB jet activity. In constrast, the lack of detectable X-ray emission from Hen 2-99 suggests that this PN has yet to enter a phase of strong wind-wind shocks.

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Section: Indeed Among the Prototype [Wcl] Objects Is Bd +30mentioning

confidence: 99%