Red Horizontal Branch and Early Asymptotic Branch Stars Near the Sun.

Details Red Horizontal Branch and Early Asymptotic Branch Stars Near the Sun. Red Horizontal Branch and Early Asymptotic Branch Stars Near the Sun.

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aj....114.1666e&link_type=abstract

The Astronomical Journal, v. 114, p. 1666.

Astronomy and Astrophysics

Astronomy

4

Stars: Horizontal-Branch, Galaxy: Abundances, Galaxy: Halo, Stars: Evolution, Stars: Agb

Scientific paper

Sixty one red horizontal branch (RHB) and early asymptotic branch (EAGB) stars are isolated. Heavy element abundances, from Strömgren photometry, and calcium abundances, from hk photometry, have been derived. The (b - y) colors of these objects are apparently not appreciably affected by differential line-blanketing although abundance determination from the m1 index of Strömgren photometry is apparently valid. The Ca abundance is derived from P[Ca/h] = [hk(obs) - hk(comp)]/0.362+0.10 dex, where hk(comp) = 1.55(b -y) + 0.335. The overabundance of the α process element calcium, with respect to the heavy elements, that was noted elsewhere for halo giants and dwarfs, is also a feature of RHB and EAGB stars. The data from the best observed halo globular clusters lead to Mυ=5.05-4.70(B - V)+[l.34-0.50(B-V)] [Fe/H] for the RHB and EAGB stars or dMυ(AGB)/d[Fe/H]=0.84 at B-V = +1.0 mag compared with 0.40 for the cluster variables in the same clusters. More recent determinations of moduli for several of the globular clusters (Reid 1997, ApJ, preprint) give values that are systematically 0.50-0.55 mag larger, effecting the zero point of the luminosity-color-abundance relation. Evidence for kinematic and abundance boundaries between disk and halo populations is discussed.

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