The anomalous giant branch of NGC 188

Details The anomalous giant branch of NGC 188 The anomalous giant branch of NGC 188

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..890t&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Mar. 15, 1978, p. 890-901.

Astronomy and Astrophysics

Astrophysics

38

Abundance, Giant Stars, Late Stars, Star Clusters, Stellar Evolution, Stellar Mass Ejection, Chemical Evolution, Cn Emission, Helium, Stellar Luminosity, Ubv Spectra

Scientific paper

The giant branch of NGC 188 has been analyzed relative to that of M67, and it is shown that a significant difference exists between the two clusters in that the giant branch of NGC 188 is intrinsically redder than the giant branch of M67. It is concluded that the most probable cause of the difference and of the observed scatter in the more luminous region of the giant branch in NGC 188 is the combined effect of mass loss, both early in post-main-sequence evolution and at the tip of the giant branch, and a difference in chemical composition between the two clusters; NGC 188 has lower helium and/or higher CNO abundance than M67. The effect of this on the ages and distance moduli of the clusters is discussed.

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