Comparisons of the HR diagrams of the youngest clusters in the Galaxy, the LMC and SMC - Evidence for a large MS widening

Details Comparisons of the HR diagrams of the youngest clusters in the Galaxy, the LMC and SMC - Evidence for a large MS widening Comparisons of the HR diagrams of the youngest clusters in the Galaxy, the LMC and SMC - Evidence for a large MS widening

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...108..148m&link_type=abstract

Astronomy and Astrophysics, vol. 108, no. 1, Apr. 1982, p. 148-156.

Astronomy and Astrophysics

Astrophysics

68

Hertzsprung-Russell Diagram, Magellanic Clouds, Star Clusters, Stellar Evolution, Supermassive Stars, B Stars, O Stars, Stellar Mass Ejection, Stellar Models

Scientific paper

A comparative analysis of the colour magnitude diagrams of 23 well observed very young clusters (age less than 2 1 O yr) is performed for four locations: clusters towards the galactic centre, the galactic anticentre, in the LMC and SMC.
The relative numbers of stars outside the band of OB stars appear to increase considerably in the sequence of the four considered zones. In particular, we note that the relative frequency of F, G, K, and M stars increases with decreasing metallicity.
Comparing models and observations of galactic clusters, properly accounting for tracks with mass loss and bolometric corrections, we find that too many stars are observed (40 % instead of 8 %) outside the MS band. Everything occurs as if the MS band were much wider than expected: it apparently reaches spectral type A. Extended internal mixing as well as atmospheric effects may be responsible for the observed MS widening.

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