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Astron. Astrophys. 362, 673-682 (2000)

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7. Conclusions

Despite the availability of consistent and more accurate photometric light curves and radial velocity curves of both components, BF Aurigae remains a difficult system for determining the mass ratio. Fits of similar quality are achieved for [FORMULA] with a slight preference derived from the line ratios for [FORMULA] yielding [FORMULA] and [FORMULA]. The absolute masses are confined to the intervals [FORMULA] and [FORMULA].

BF Aur is best understood as a pair of evolved stars of spectral type B5V, of which the more massive component (the spectroscopic primary or photometric secondary, respectively) now almost fills its Roche lobe. Although BF Aur may be on the verge of becoming an inverse Algol (the configuration suggested by Schneider et al. 1979), interactions are of small scale and Roche lobe overflow probably has not yet fully developed.

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© European Southern Observatory (ESO) 2000

Online publication: October 24, 2000
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