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Empirical bolometric corrections for the main-sequence
Empirical relations are derived between the bolometric corrections andmasses, spectral types and effective temperatures of main sequencestars. The most reliable available data for visual/astrometric binariesand eclipsing binaries that are at the same time double-linesspectroscopic binaries was used to obtain empirical mass-spectral typeand mass-visual luminosity relations for the first group, and empiricalmass-gravity, mass-radius, mass-spectral type, mass-effectivetemperature and mass-bolometric luminosity relations for the second. Amean mass-bolometric correction relation is then derived for the entirerange of main sequence stars which may be transformed into relationsbetween the bolometric correction and spectral type or effectivetemperature. The results are found to agree well with the theoreticalresults of Buser and Kurucz (1978) for masses greater than 7 solarmasses and equal to 1.35 solar masses, and with the empirical results ofCode et al. (1976).
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Observation and Astrometry data
| Constellation: | Βοώτης |
| Right ascension: | 14h45m20.21s |
| Declination: | +20°09'22.4" |
| Apparent magnitude: | 8.658 |
| Distance: | 172.414 parsecs |
| Proper motion RA: | -45.8 |
| Proper motion Dec: | 22 |
| B-T magnitude: | 9.152 |
| V-T magnitude: | 8.699 |
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