Astrophysical properties of red giants in three open clusters older than the Hyades

Details Astrophysical properties of red giants in three open clusters older than the Hyades Astrophysical properties of red giants in three open clusters older than the Hyades

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983japa....4..117c&link_type=abstract

Journal of Astrophysics and Astronomy (ISSN 0250-6335), vol. 4, June 1983, p. 117-134. Research supported by the Consejo Naciona

Astronomy and Astrophysics

Astrophysics

41

Abundance, Late Stars, Open Clusters, Red Giant Stars, Stellar Spectrophotometry, Astrophysics, Electrophotometry, Metallicity, Stellar Mass, Stellar Temperature

Scientific paper

The application to the program stars of two independent membership criteria based on BV and DDO photometry makes it possible to distinguish a few red field stars from the physical members of the clusters. In particular, two stars previously thought to be members of NGC 3680 by Eggen (1969) and McClure (1972) are found not to be physically connected with this cluster. It is also found that the cluster giants in NGC 2482 and IC 4651 have CN strengths nearly identical with the Hyades giants, whereas NGC 3680 is considerably poorer in CN than the above clusters. Within the limits of the DDO photometry, no firm evidence is seen for any intrinsic differences in CN strength among the giants in the three clusters. This result is valid for the clump stars at the blue end of the giant branch in NGC 3680 and IC 4651. Both CMT(1)T(2) and DDO data lend support to the conclusion that IC 4651 is on the metal-rich side of the distribution of intermediate and old open clusters. The mass results indicate that the clumps stars in NGC 3680 and IC 4651 could have undergone mass loss before reaching their core burning phase of evolution.

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