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On the interpretation of Stromgren photometry
It is shown that at least four parameters are needed to explain theintrinsic colors of G dwarfs very accurately. This limits the precisionwith which forbidden Fe/H and surface gravity can be estimated fromStromgren photometry alone. Definite conclusions as to the origin of theHyades anomaly must await more precise model atmospheres and a moreaccurate knowledge of the chemical composition of the stars concerned;however, it is likely that most of the anomaly can be attributed todifferences in line blanketing. In particular, there appears to be nogood evidence at present to suggest that the helium abundance of theHyades is less than that of the Coma cluster or Ursa Major nucleus.Observations indicate that the Swan bands of C2 are much stronger inHyades dwarfs than in dwarfs of the same temperature in either of theother two clusters. Photometric observations of the components of anoutlying wide binary in the Hyades suggest that the initial chemicalcomposition of these stars is somewhat different from that of typicalmembers of the cluster.
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Observation and Astrometry data
| Constellation: | Ωρολόγιον |
| Right ascension: | 03h13m41.85s |
| Declination: | -65°49'48.3" |
| Apparent magnitude: | 8.483 |
| Distance: | 127.389 parsecs |
| Proper motion RA: | -17.6 |
| Proper motion Dec: | -20 |
| B-T magnitude: | 9.102 |
| V-T magnitude: | 8.535 |
Catalogs and designations:
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