Hostname: page-component-77c89778f8-5wvtr Total loading time: 0 Render date: 2024-07-17T10:23:04.577Z Has data issue: false hasContentIssue false
  • English
  • Français

The Hyades Cluster — Solar Metallicity?

Published online by Cambridge University Press:  14 August 2015

Phillip J. Flower
Phillip J. Flower*
Affiliation:
Department of Physics and Astronomy, Clemson University, Clemson SC 29631

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Some simple comparisons have been made between models of main sequence (MS) stars and the Hyades main sequence with the aim of investigating the effects of small changes in the stellar opacities, the zero point of the temperature scale and the assumed distance modulus for Hyades cluster have on the inferred metallicity of the Hyades. Three grids of MS models were constructed using the Cox and Stewart (1970a,b) opacities. Furthermore, taking a rather conservative view with regard to future changes in opacity compilations, another grid was constructed with opacities 20% higher than the Cox-Stewart opacities. Following the procedure outlined by Gough and Weiss (1976), the mixing length required for constructing a solar model was found to be 1.36. Because recent photometric and spectroscopic work (Barry et al. 1978; Hardorp 1978) suggests that the sun may be redder than traditionally believed, i.e., (B-V)⊙ = 0.66–0.67 instead of 0.63 mag, two temperature scales have been used to transform the MS models to the CM diagram.

Type
August 27 Introduction, Associations, Galactic Structure
Information
Symposium - International Astronomical Union , Volume 85: Star Clusters , 1980 , pp. 119 - 120
Copyright
Copyright © Reidel 1980 

References

Barry, D.C., Cromwell, R.H. and Schoolman, S.A.: 1978, Astrophys. J. 222, 1032.CrossRefGoogle Scholar
Cox, A.N. and Stewart, J.N.: 1970a, Astrophys. J. Suppl 19, 243.Google Scholar
Cox, A.N. and Stewart, J.N.: 1970b Astrophys. J. Suppl. 19, 261.Google Scholar
Flower, P.J. 1978, in Philip, A.G.D. and Hayes, D. S. (eds.), IAU Symp. No. 80: The HR Diagram, Reidel, Dordrecht, p. 151.Google Scholar
Gough, D.O. and Weiss, N.O.: 1976, Mon. Not. Roy. Astron. Soc. 176, 589.Google Scholar
Hardorp, J.: 1978, Astron. Ap. 63, 383.Google Scholar
Nicolet, B.: 1978, Astron. Ap. Suppl. 34, 1.Google Scholar
Perrin, M.N., Hejlesen, P.M., Cayrel de Strobel, G., and Cayrel, R.: 1977, Astron. Astrophys. 54, 779.Google Scholar
Taylor, B.J.: 1978, Astrophys. J. Suppl. 36, 173.Google Scholar