Radial metal variation as possible explanation of colour gradients in the cores of globular clusters

Details Radial metal variation as possible explanation of colour gradients in the cores of globular clusters Radial metal variation as possible explanation of colour gradients in the cores of globular clusters

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....96..254a&link_type=abstract

Astronomy and Astrophysics, vol. 96, no. 1-2, Mar. 1981, p. 254-258.

Astronomy and Astrophysics

Astrophysics

5

Abundance, Astronomical Models, Color, Globular Clusters, Metallic Stars, Radial Distribution, A Stars, Astronomical Photometry, B Stars, Cores, Cosmic Dust

Scientific paper

Recently reported observational data (Chun and Freeman, 1979) showed the occurrence of radial colour gradients in the cores of some globular clusters. In a previous paper (Angeletti et al., 1980) we investigated the consequences of the existence of small central dust clouds in models of globulars. In the present paper we study the suggestion that those colour gradients might be caused by radial variations of the metal abundance (Z =10-3 at the centre, Z = 10-4 in the halo). In both approaches we proceeded tentatively, that is we studied various cases with a certain number of free parameters and then selected those cases that matched better the observed colour profiles. Cluster models consisting of a central nucleus with metal-rich stars, an intermediate region with stars with a variable metal abundance, and a halo with metal poor-stars appeared plausible. However, the hypothesis of a metal gradient is not necessarily alternative to that of a dust cloud. Rather, it may be concluded tentatively that the two possibilities are complementary to each other. In this manner one might also explain the observed pattern of colour profiles in globular clusters.

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