On the interpretation of Stromgren photometry

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Abstract
It is shown that at least four parameters are needed to explain the intrinsic colors of G dwarfs very accurately. This limits the precision with which forbidden [Fe/H] and surface gravity can be estimated from Strömgren photometry alone. Definite conclusions as to the origin of the Hyades anomaly must await more precise model atmospheres and a more accurate knowledge of the chemical composition of the stars concerned; however, it is likely that most of the anomaly can be attributed to differences in line blanketing. In particular, there appears to be no good evidence at present to suggest that the helium abundance of the Hyades is less than that of the Coma cluster or Ursa Major nucleus. Observations indicate that the Swan bands of C2 are much stronger in Hyades dwarfs than in dwarfs of the same temperature in either of the other two clusters. Photometric observations of the components of an outlying wide binary in the Hyades suggest that the initial chemical composition of these stars is somewhat different from that of typical members of the cluster.

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