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Low Mass Wolf-Rayet Stars: Theory

Published online by Cambridge University Press:  14 August 2015

Alvio Renzini
Alvio Renzini*
Affiliation:
Osservatorio Astronomico, CP 596, 40100 Bologna, Italy

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It is well known that the Wolf-Rayet phenomenon is not restricted to some bright and massive stars, presumably in their core hydrogen-burning or helium-burning phase, but that it is also encountered among the central stars of some planetary nebulae (PNe). The PN nuclei are generally regarded as the evolutionary product of low and intermediate mass stars (with initial masses M.1 below ∼5 M⊙), which have lost most of their hydrogen-rich envelope during the so-called Asymptotic Giant Branch (AGB) phase. Correspondingly, their present mass cannot exceed the Chandrasekhar limit (∼1.4 M⊙), and their internal structure consists of a highly degenerate carbon-oxygen core containing most of the stellar mass, surrounded by an intershell region of mass ΔMCSH, and by a very low-mass envelope (Me < ∼10−3 M⊙).

Type
SESSION 6 — LOW MASS WOLF-RAYET STARS RING NEBULAE
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 413 - 422
Copyright
Copyright © Reidel 1982 

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