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The stellar temperature scale from O5 to A0

Published online by Cambridge University Press:  14 August 2015

D.S. Hayes
D.S. Hayes*
Affiliation:
Dept. of Physics and Astronomy, Rensselaer Polytechnic Institute, Troy, N.Y., U.S.A.

Abstract

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An absolute spectrophotometric calibration of Vega and eleven other standard stars was completed by the author in 1967. This calibration extends from 3200 to 10870 Å, and therefore gives a useful calibration of the Paschen discontinuity as well as the Balmer discontinuity, for which calibrations have been available for some time.

The measured values of the ratio of the size of the Paschen discontinuity to the size of the Balmer discontinuity have been compared with corresponding values predicted by model atmospheres. The comparison shows that LTE models satisfactorily predict the continuum in the wavelength range given above.

A stellar temperature scale has been determined by fitting the measured sizes of the Balmer discontinuity of 43 stars to blanketed model atmospheres. This temperature scale agrees very well with Morton's modified form of the Morton-Adams temperature scale for all except the latest B-stars, for which higher temperatures are predicted.

Type
Part I: Stellar Fluxes
Information
Symposium - International Astronomical Union , Volume 36: Ultraviolet Stellar Spectra and Related Ground-Based Observations , 1970 , pp. 83 - 89
Copyright
Copyright © Reidel 1970 

References

Adams, T. F. and Morton, D. C.: 1968, Astrophys. J. 152, 195.CrossRefGoogle Scholar
Bahner, K.: 1963, Astrophys. J. 138, 1314.CrossRefGoogle Scholar
Barbier, D.: 1955, ‘Principes fondamentaux de classification stellaire’, Colloques Int. Centre Nat. Rech. Sc., Paris, 55, 47.Google Scholar
Bless, R. C., Code, A. D., and Houck, T. E.: 1968, Astrophys. J. 153, 561.CrossRefGoogle Scholar
Bradley, P. T. and Morton, D. C.: 1969, Astrophys. J. 156, 687.CrossRefGoogle Scholar
Brown, R. Hanbury, Davis, J., Allen, L. R., and Rome, J. M.: 1967, Monthly Notices Roy. Astron. Soc. 137, 393.CrossRefGoogle Scholar
Chalonge, D. and Divan, L.: 1952, Ann. Astrophys. 15, 201.Google Scholar
Collins, G. W. II: 1968, Astrophys. J. 152, 847.CrossRefGoogle Scholar
Divan, L.: 1966, IAU Symposium 24: Spectral Classification and Multicolour Photometry (ed. by Loden, K., Loden, L. O., and Sinnerstad, U.), Academic Press, London and New York, p. 311.Google Scholar
Harris, D. L. III: 1963, ‘The Stellar Temperature Scale and Bolometric Corrections’ in Stars and Stellar Systems, Vol. III, Basic Astronomical Data (ed. by Strand, K. Aa.), University of Chicago Press, Chicago, p. 263.Google Scholar
Hayes, D. S.: 1967, Unpublished Ph.D. dissertation, University of California at Los Angeles.Google Scholar
Hayes, D. S.: 1970, Astrophys. J. 159, 165.CrossRefGoogle Scholar
Hickok, F. R. and Morton, D. C.: 1968, Astrophys. J. 152, 203.CrossRefGoogle Scholar
Johnson, H. L.: 1966, Ann. Rev. Astron. Astrophys. 4, 193.CrossRefGoogle Scholar
Johnson, H. L., Mitchell, R. I., Iriarte, B., and Wisniewski, W. Z.: 1966, Comm. Lun. Planet. Lab. 4, 99.Google Scholar
Mihalas, D.: 1964, Astrophys. J. Suppl. Ser. 9, 321.CrossRefGoogle Scholar
Mihalas, D.: 1968, Astrophys. J. 153, 317.CrossRefGoogle Scholar
Mihalas, D. M. and Morton, D. C.: 1965, Astrophys. J. 142, 253.CrossRefGoogle Scholar
Mitchell, R. I. and Johnson, H. L.: 1969, Comm. Lun. Planet. Lab. 8, 1.Google Scholar
Morton, D. C. and Adams, T. F.: 1968, Astrophys. J. 151, 611.CrossRefGoogle Scholar
Whiteoak, J. B.: 1966, Astrophys. J. 144, 305.CrossRefGoogle Scholar
Wolff, S. C., Kuhi, L. V., and Hayes, D.: 1968, Astrophys. J. 152, 871.CrossRefGoogle Scholar