Astronomy and Astrophysics – Astronomy
Scientific paper
May 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986pasp...98..473l&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 98, May 1986, p. 473-485. Research supported by the Cal
Astronomy and Astrophysics
Astronomy
94
Carbon Stars, Globular Clusters, Stellar Composition, Subgiant Stars, Abundance, Color-Magnitude Diagram, Nitrogen, Stellar Spectrophotometry
Scientific paper
The authors find that >[C/Fe]< ≈ 0.0 in stars at the base of the subgiant branch and approaches +0.1 in stars near the main-sequence turnoff in the metal-poor globular cluster M92. The carbon abundance falls on the average by about 0.5 dex by the time stars reach MV0 ≡ +1.5. These carbon depletions occur early enough and are approximately the right size to account for the large average nitrogen enhancement ([N/Fe] ≡ +0.65) observed in M92 subgiants near MV0 ≡ +1.5. Although the present observations do not absolutely prove that C→N conversion and mixing alone control the C- and N-abundances seen in M92 giants, neither is there any longer a compelling reason to believe there were large primordial nitrogen abundance variations in M92. The mechanism responsible for the large (Δ[C/Fe] ≈ 1.0) carbon depletions observed as stars ascend the M92 giant branch to the red-giant tip remains unknown.
Carbon Duane F.
Friel Eileen
Kraft Ralph Porter
Langer Edward G.
Oke Bev J.
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