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The Absolute Magnitudes of the Nearby Stars: Calibrations of mean luminosity relations
Published online by Cambridge University Press: 04 August 2017
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The nearby stars are most favored for determining precise absolute magnitudes and for calibrating spectral-type, luminosity relations and color, luminosity relations. To demonstrate the main problems we discuss the (Mv,B-V) relation since (B-V) data are available for most of our candidates. At Yale Observatory van Altena is compiling a new catalog of trigonometric parallaxes. We feel deeply indebted to van Altena for making available to us a preliminary version of this catalog.
- Type
- Research Article
- Information
- Symposium - International Astronomical Union , Volume 111: Calibration of Fundamental Stellar Quantities , 1985 , pp. 369 - 372
- Copyright
- Copyright © Reidel 1985
References
Calibrations of absolute magnitudes for nearby stars used up to now are published in.Google Scholar
Jahreiss, H. and Gliese, W.
1983, in Statistical Methods in Astronomy, ed. Rolfe, E. J., (ESA Spec. Publ., SP-201), p. 201.Google Scholar
The theoretical aspects of the calibration of absolute magnitudes from trigonometric parallaxes are described by.Google Scholar
Lutz, T. E.
1983, in IAU Colloquium No. 76, The Nearby Stars and the Stellar Luminosity Function, ed. Philip, A. G. D. and Upgren, A. R., (L. Davis Press, Schenectady), p. 41.Google Scholar
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