[WN] central stars of planetary nebulae

Todt, H.; Miszalski, B.; Toalá, J. A.; Guerrero, M. A.

doi:10.1017/s1743921317000540

Cited by 1 publication

(3 citation statements)

References 15 publications

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“…This feature is seen both in our restricted sample with definite spectral types (our "pure" sample), as well as in the complete sample that includes also uncertain spectral types. This result is consistent with previous results in the literature Todt (2009). Even more, given that our sample is significantly larger than that discussed by Todt (2009), we consider this result as a confirmation that the lack of subtypes 5-7 in [WR]-CSPNe is a real feature.…”

Section: Dichotomy Between H Rich and Poor Cspnesupporting

confidence: 94%

“…This result is consistent with previous results in the literature Todt (2009). Even more, given that our sample is significantly larger than that discussed by Todt (2009), we consider this result as a confirmation that the lack of subtypes 5-7 in [WR]-CSPNe is a real feature. In principle this gap could be explained in two different ways.…”

Section: Dichotomy Between H Rich and Poor Cspnesupporting

confidence: 94%

“…Consequently, the evolutionary state is not clear. One possibility is that [WN] → O(He) (Todt et al 2017).…”

Section: Review Of Stellar Evolutionmentioning

confidence: 99%

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Catalogue of the central stars of planetary nebulae

Weidmann

Mari

Schmidt

et al. 2020

A&A

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Planetary nebulae represent a potential late stage of stellar evolution, however, their central stars (CSPNe) are relatively faint and, therefore, pertinent information is available for merely < 20% of the Galactic sample. Consequently, the literature was surveyed to construct a new catalogue of 620 CSPNe featuring important spectral classifications and information. The catalogue supersedes the existing iteration by 25% and includes physical parameters such as luminosity, surface gravity, temperature, magnitude estimates, and references for published spectra. The marked statistical improvement enabled the following pertinent conclusions to be determined: the H-rich/H-poor ratio is 2:1, there is a deficiency of CSPNe with types [WC 5-6], and nearly 80% of binary central stars belong to the H-rich group. The last finding suggests that evolutionary scenarios leading to the formation of binary central stars interfere with the conditions required for the formation of H-poor CSPN. Approximately 50% of the sample with derived values of log L⋆, log Teff, and log g, exhibit masses and ages consistent with single stellar evolutionary models. The implication is that single stars are indeed able to form planetary nebulae. Moreover, it is shown that H-poor CSPNe are formed by higher mass progenitors. The catalogue is available through the Vizier database.

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Section: Dichotomy Between H Rich and Poor Cspnesupporting

confidence: 94%

Section: Dichotomy Between H Rich and Poor Cspnesupporting

confidence: 94%