The evolution of large planetary nebulae and their central stars

Kaler, J. B.

doi:10.1086/161188

Cited by 149 publications

(114 citation statements)

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“…The spectral energy distribution, constructed from all four measurements imply that the bulk of the radio emission, up to 14.7 GHz, is coming from an optically thick environment. However, the calculated brightness temperature at 1.4 GHz of T b ≈ 2 K and excellent agreement with the flux predicted from Hβ (from Kaler (1983)) imply optically thin free-free emission at frequencies ν > 1 GHz. One can argue that both NVSS and ATCA flux measurements could be affected by the missing flux problem due to the relatively large angular size of this PN (θ opt ≈ 60 ′′ ).…”

Section: Abell 51 (Png0176-102)supporting

confidence: 76%

A pilot study of the radio‐continuum emission from MASH planetary nebulae

et al. 2011

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Key words astronomical data bases: miscellaneous -planetary nebulae: general -radiation mechanisms: thermal -radio continuum: ISM We report an Australia Telescope Compact Array (ATCA) radio-continuum observations of 26 planetary nebulae (PNe) at wavelengths of 3 and 6 cm. This sample of 26 PNe were taken from the Macquarie/AAO/Strasbourg Hα PNe (MASH) catalogue and previous lists. We investigate radio detection quality including measured and derived parameters for all detected or marginally detected PNe from this combined sample. Some 11 objects from the observed sample have been successfully detected and parametrized. Except for one, all detected PNe have very low radio surface brightnesses. We use a statistical distance scale method to calculate distances and ionised masses of the detected objects. Nebulae from this sample are found to be large (>0.2 pc in diameter) and highly diluted which indicates old age. For 21 PNe from this sample we list integrated Hα fluxes and interstellar extinction coefficients, either taken from the literature or derived here from the Balmer decrement and radio to Hα ratio methods. Finally, our detected fraction of the MASH pilot sample is relatively low compared to the non-MASH sub-sample. We conclude that future radio surveys of the MASH sample must involve deeper observations with better uv coverage in order to increase the fraction of detected objects and improve the quality of the derived parameters.

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Section: Abell 51 (Png0176-102)supporting

confidence: 76%

A pilot study of the radio‐continuum emission from MASH planetary nebulae

et al. 2011

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“…Borkowski, & Tsvetanov 1995) showed nebular C iv absorption. As the He ii or H Zanstra temperatures of their central stars are ∼50,000 K and ∼70,000 K, respectively (Kaler & Jacoby 1991;Kaler 1983), these observations are not useful for the study of 10 5 K gas. N v lines have small oscillator strengths, so are difficult to detect.…”

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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“…The conventional method (known as the Zanstra method) is to derive the central-star temperature from a comparison of the nebular recombination flux with the stellar continuum magnitude. This method has been applied to more than 300 nebulae (Kaler 1983;Pottasch 1984;Shaw and Kaler 1989;Gleizes, Acker, and Stenholm 1989;Gathier and Pottasch 1989). Since the Zanstra method assumes that the nebula is optically thick, and PNe change from optically thick to optically thin in hydrogen and helium at different times, this can lead to different estimates of the central-star temperature by using hydrogen or helium lines.…”

Section: Central-star Temperaturesmentioning

confidence: 99%

“…The fact that stellar atmospheres are not well approximated by blackbodies can also contribute to errors in the Zanstra temperatures (Henry and Shipman 1986). However, it can be argued that since PNe central stars have a large variety of spectral types and abundances, the blackbody assumption is probably no worse than any specific set of atmosphere models (Kaler 1983). …”

Section: Central-star Temperaturesmentioning

confidence: 99%

Planetary nebulae: A modern view

Kwok

1994

PASP

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ABSTRACT. Our current understanding of the origin and evolution of planetary nebulae is reviewed. We now recognize that a planetary nebula represents a dynamical system in which evolution is tightly coupled to the evolution of the central star. Not only is the ionization structure of the nebula controlled by the radiative output from the central star, the dynamics and morphology of the nebula are heavily influenced by the mechanical energy output from the central star. Since the time scale of evolution of the central star is strongly dependent on its mass, the extent of the radiative and mechanical interactions between the star and the nebula not only vary with time, but also vary with stellar mass. The physical properties of planetary nebulae are discussed in this context.

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The evolution of large planetary nebulae and their central stars

Cited by 149 publications

References 0 publications

A pilot study of the radio‐continuum emission from MASH planetary nebulae

A pilot study of the radio‐continuum emission from MASH planetary nebulae

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

Planetary nebulae: A modern view

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