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[WC] and PG1159 Central Stars of Planetary Nebula: the Need for an Alternative to the Born-Again Scenario
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Hydrogen-deficient central stars of planetary nebula such as Wolf-Rayet and PG1159 central stars and some weak emission line stars are primarily composed of helium and carbon. This abundance is well explained by a scenario where a single post-AGB star experiences a last helium shell flash which ingests and burns, or simply dilutes, the remaining hydrogen atmosphere. But despite its success in matching the photospheric abundances of these stars, this scenario is faced with several observational challenges. A binary scenario is proposed here as a more natural way to face some of the most stringent observational constraints. In this scenario the H-rich primary in a close binary formed during a common envelope on the AGB, suffers a last helium shell flash, which results in a H-deficient primary with some of the characteristics needed to match the observations.
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Cited by 2 Pith papers
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Infrared properties of Planetary Nebulae with PG1159 central stars
A systematic infrared analysis of PG1159 planetary nebulae finds cooler dust and lower dust masses than other hydrogen-poor nebulae and suggests an evolutionary sequence from [WRE] to PG1159 central stars based on H b...
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A primer on the formation and evolution of hydrogen deficient Central Stars of Planetary Nebul{\ae} and Related Objects
A review of the formation and evolution of hydrogen-deficient central stars of planetary nebulae, comparing late thermal pulse (born again) and binary merger channels.
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