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Effects of Stellar Rotation on Spectral Classification

Published online by Cambridge University Press:  12 April 2016

Arne Slettebak  and
Thomas J. Kuzma
Arne Slettebak
Affiliation:
Perkins Observatory, Ohio State and Ohio Wesleyan Universities
Thomas J. Kuzma
Affiliation:
Perkins Observatory, Ohio State and Ohio Wesleyan Universities

Abstract

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Stellar rotation may affect the strengths of lines used in spectral classification because of effects of plate resolution and also because of physical changes in the rotating stellar atmospheres. In the first case, the importance of using standard stars with appropriate rotational line broadening in classifying spectra of relatively high dispersion (resolution) is emphasized. Rotational effects on weak lines in general and on the Balmer lines may cause systematic errors in the assignment of spectral types and luminosity classes unless the standard stars are chosen with line broadening similar to that of the star to be classified. With regard to physical changes in the rotating atmospheres, we have extended the earlier work of Collins to include the Balmer lines plus additional lines of He I and Si II which are important in spectral classification over a wider range of spectral types.

Type
II Criteria and Applications of MK Classification
Information
International Astronomical Union Colloquium , Volume 47: Spectral Classification of the Future , 1979 , pp. 87 - 94
Copyright
Copyright © Vatican Observatory 1979

References

Abt, H.A. (1963). Astrophys. J. Suppl. 8, 99.Google Scholar
Baiona, L.A. (1975). Monthly Not. Roy. Astron, Soc. 173, 449.Google Scholar
Collins, G.W. II. (1968a). Astrophys. J. 151, 217.Google Scholar
Collins, G.W. II. (1968b). Ibid. 152, 847.Google Scholar
Collins, G.W. II. (1970). In Stellar Rotation, Slettebak, A., ed., Reidel: Dordrecht, p. 85.Google Scholar
Collins, G.W. II. (1974). Astrophys. J. 191, 157.Google Scholar
Collins, G.W. II. and Harrington, J.P. (1966). Astrophys. J. Suppl. 146, 152.CrossRefGoogle Scholar
Collins, G.W. II. and Sonneborn, G.H. (1977). Astrophys. J. Suppl. 34, 41.Google Scholar
Friedjung, M. (1968). Astrophys. J. 151, 779.Google Scholar
Gieske, H.A. and Griem, H.R. (1969). Astrophys. J. 157, 963.Google Scholar
Griem, H.R. (1974). In Spectral Line Broadening by Plasmas. Academic Press: New York.Google Scholar
Hardorp, J. and Scholz, M. (1971). Astron. and Astrophys. 13, 353.Google Scholar
Hardorp, J. and Strittmatter, P.A. (1968). Astrophys. J. 153, 465.Google Scholar
Jaschek, C. (1970). In Stellar Rotation, Slettebak, A., ed., Reidel: Dordrecht, p. 219.Google Scholar
Keenan, P.C. (1963). In Stars and Stellar Systems, Vol. III: Basic Astronomical Data. Strand, K.Aa. ed., University of Chicago Press: Chicago, p. 78.Google Scholar
Morgan, W.W., Keenan, P.C. and Kellman, E. (1943). In An Atlas of Stellar Spectra, University of Chicago Press: Chicago.Google Scholar
Stoeckley, T.R. and Mihalas, D. (1973). NCAR-TN/STR-81t, Natl. Cent. Atmos. Res,: Boulder.Google Scholar
Warren, W.H. (1976). Monthly Not. Roy. Astron. Soc. 174, 111.Google Scholar