Evolution, Nucleosynthesis, and Pulsation of AGB Stars

  • John C. Lattanzio
  • Peter R. Wood
Part of the Astronomy and Astrophysics Library book series (AAL)

Abstract

The Hertzsprung-Russell diagrams of low metallicity globular clusters provide excellent demonstrations of the asymptotic giant branch, or AGB. The HR-diagram of M3, shown in Figure 2.1, is a good example. When HR-diagrams such as Figure 2.1 were first obtained in the 1950s, the asymptotic merging of the AGB and the red giant branch (RGB) was regarded as a “bifurcation” viewed looking down from the tip of the giant branch (e.g., Sandage [123]; Arp [7]). At this stage the direction of evolution was unknown. Probably the first authors to use the term “asymptotic” were Sandage and Walker [124]. This was just after Schwarzschild and Härm [129] had evolved a low mass star past the Horizontal Branch and up the AGB. Although the term asymptotic giant branch originated as a description of the sequence of stars in the HR diagrams of low-mass globular cluster stars, the term is now generally used to describe all stars with masses ≲ 8 M that are on the second ascent into the red giant region of the HR-diagram.

Keywords

Light Curf Globular Cluster Asymptotic Giant Branch Carbon Star Thermal Pulse 
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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Copyright information

© Springer Science+Business Media New York 2004

Authors and Affiliations

  • John C. Lattanzio
    • 1
  • Peter R. Wood
    • 2
  1. 1.School of Mathematical SciencesMonash UniversityAustralia
  2. 2.Research School of Astronomy and AstrophysicsAustralian National UniversityAustralia

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