The degree of completeness of nearby stars and the stellar luminosity function

Details The degree of completeness of nearby stars and the stellar luminosity function The degree of completeness of nearby stars and the stellar luminosity function

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981aj.....86.1898u&link_type=abstract

Astronomical Journal, vol. 86, Dec. 1981, p. 1898-1908.

Astronomy and Astrophysics

Astronomy

52

Mass To Light Ratios, Star Distribution, Stellar Luminosity, Stellar Spectra, M Stars, Main Sequence Stars, O Stars, Spatial Distribution, Stellar Magnitude, Stellar Motions, Sun, Ubv Spectra

Scientific paper

The aim of this study is the determination of the degree of completeness of nearby star catalogs for stars of as many spectral classes as possible, by means of a novel method which eliminates giants, subgiants and white dwarfs from the data sample. It is shown that main-sequence stars earlier than M0 are essentially complete and identified within about 20 pc of the sun, by determining V/V(max) as a function of B-V for the main sequence stars. The luminosity function produced by the M0 stars has been known to differ from the commonly accepted and smoothed luminosity function, which increases monotonically with absolute magnitude, between the absolute visual magnitudes +6 and +9. It is concluded that the deficiency between these magnitude limits is real, suggesting either (1) that stars of masses equivalent to this absolute magnitude range are rarer than those of greater mass, or (2) that the mass-luminosity relation is not as linear as is believed at present.

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