Colour gradients in globular clusters

Details Colour gradients in globular clusters Colour gradients in globular clusters

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119..279p&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 119, no. 2, Feb. 1986, p. 279-285. CNPq-supported research.

Astronomy and Astrophysics

Astrophysics

3

Abundance, Globular Clusters, Stellar Color, Stellar Spectrophotometry, Electrophotometry, Gradients, Hertzsprung-Russell Diagram, Ubv Spectra

Scientific paper

Radial color gradients in the globular clusters NGC 2808, NGC 1851, NGC 5139, NGC 6388, NGC 6441, NGC 6541, NGC 6723, and NGC 7099 were searched by B-V and DDO photoelectric photometry, using a set of circular diaphragms. Two of the observed globular clusters, NGC 5139 (Omega Cen) and NGC 7099 (M30), showed B-V and C(45-48) color gradients; the color C(42-45) is essentially constant in these clusters, which means that the physical reason for those gradients cannot be attributed to chemical composition variations, since C(42-45) is a good metal abundance indicator. B-V colors in the external regions of NGC 5139 and NGC 7099 were obtained by synthesizing the observed HR diagrams of these clusters. The ages and the relaxation times for NGC 5139 and NGC 7099 indicate that mass segregation must have taken place in both clusters, which is probably related to the observed color gradients.

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