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AGB Stars in Binaries and Their Progeny

  • Alain Jorissen
Part of the Astronomy and Astrophysics Library book series (AAL)

Abstract

Although binarity and AGB evolution are in principle disconnected concepts (a star need not be member of a binary system to evolve along the AGB), a rich world flourishes at their contact. The interest in discussing binary stars with an AGB component goes far beyond the possibility of deriving their masses. First, binarity is expected to alter the intrinsic properties of AGB stars (pulsation, mass loss, dust formation, etc.). Second, the importance of the rich progeny of binary stars involving AGB stars has been recognized recently. Various classes of stars with peculiar abundances (such as barium stars, CH stars, Tc-poor S stars, etc.) have indeed been identified as the progeny of binary systems formerly involving an AGB star. Mass transfer from the AGB component is held responsible for the chemical anomalies now observed at the surface of the companion star, which dominates the light of the system, since the AGB star has evolved into a dim white dwarf (WD). Therefore, two broad classes of binary systems must be distinguished in relation to AGB stars: (A) The primary star1 is currently an AGB star, while the secondary is still an unevolved dwarf; (B) The secondary is a WD, while the primary is at any evolutionary stage (except WD) and has been polluted by the secondary when the latter was an AGB star.2 The present chapter is organized as follows. Sections 9.2 and 9.3 deal with case A.

Keywords

White Dwarf Roche Lobe Carbon Star Common Envelope Symbiotic Star 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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© Springer Science+Business Media New York 2004

Authors and Affiliations

  • Alain Jorissen
    • 1
  1. 1.Institut d’Astronomie et d’AstrophysiqueUniversité Libre de BruxellesBelgium

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