Abstract
In order to characterize the colour of a star by one single number we have used the colour index: m pg — m pv. This would indeed be sufficient, if the energy distribution in stellar spectra corresponded to that of black bodies. The observation shows, however, that there are considerable deviations, due to the accumulation of Fraunhofer lines, to interstellar reddening, or to differences in composition.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
References
Johnson, H. L.: 1963, in Stars and Stellar Systems, Vol. III, p. 204.
Johnson, H. L. and Morgan, W. W.: 1953, Astrophys. J. 17, 313. See also the data for clusters (B33).
Johnson, H. L.: 1955, Ann. Astrophys. 18, 292.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1987 D. Reidel Publishing Company
About this chapter
Cite this chapter
Kleczek, J. (1987). The UBV Photometric System (L). In: Kleczek, J. (eds) Exercises in Astronomy. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3769-7_43
Download citation
DOI: https://doi.org/10.1007/978-94-009-3769-7_43
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-2423-6
Online ISBN: 978-94-009-3769-7
eBook Packages: Springer Book Archive