By Alan H. Batten (auth.), D. S. Hayes, L. E. Pasinetti, A. G. Davis Philip (eds.)
Read or Download Calibration of Fundamental Stellar Quantities: Proceedings of the 111th Symposium of the International Astronomical Union held at Villa Olmo, Como, Italy, May 24–29, 1984 PDF
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Additional info for Calibration of Fundamental Stellar Quantities: Proceedings of the 111th Symposium of the International Astronomical Union held at Villa Olmo, Como, Italy, May 24–29, 1984
THE USE AND ABUSE OF STANDARD STARS R. F. Garrison David Dunlap Observatory University of Toronto ABSTRACT. Most systems of classification or quantitative measurement depend on standards. It is of the greatest importance for the user to be aware of the mandate of a particular system. If the mandate is not understood by casual users, a system can be either underutilized or abused. In tile particular case of the MK system of spectral classification, types are defined by the standard stars. They can be calibrated, and the calibration may evolve with time, but the types are relatively stable because they are defined by the standards.
The MK system of standards may not be applicable to other wavelength regions or other resolutions, but the MK process can be used to set up any classification scheme. 1 Definition of Terms In this talk, the term classification will be used in its broadest sense, including directly measured quantities. For example, the measurement of parallax allows an ordering, or "classification", of stars according to numerical parallax or distance. Most, but not all, of the classification systems in astronomy use standard stars to a greater or lesser degree.
The whole question of reference stars for cross-correlation needs careful consideration. Perhaps this should be done at the radial velocity colloquium next October. BOHLIN: Could you please describe in more detail the problems especially associated with using B stars as radial velocity standards with a precision of 1 km/sec? What are the prospects of obtaining standards with this p~ecision for the hotter stars that could be used in the UV down to 1150 A? BATTEN: The problems are the difficulty of measuring rotationally broadened spectral lines to that precision and the fact that no one knows if the velocities of B-type stars are constant to that degree.