The mass ratio and the orbital parameters of the sdOB binary AA Doradus

Abstract

The time sequence of 105 spectra covering one full orbital period of AA Dor has been analyzed. Direct determination of Vsini for the sdOB component from 97 spectra outside of the eclipse for the lines MgII 4481 A and SiIV 4089 A clearly indicated a substantially smaller value than estimated before. Detailed modelling of line profile variations for 8 spectra during the eclipse for the MgII 4481 A line, combined with the out-of-eclipse fits, gave Vsini = 31.8+/-1.8 km/s. The previous determinations of Vsini, based on the HeII 4686 A line, appear to be invalid because of the large natural broadening of the line. With the assumption of the solid-body, synchronous rotation of the sdOB primary, the measured values of the semi-amplitude K1 and Vsini lead to the mass ratio q = 0.213+/-0.013 which in turn gives K2 and thus the masses and radii of both components. The sdOB component appears to be less massive than assumed before, M1 = 0.25+/-0.05 Msol, but the secondary has its mass-radius parameters close to theoretically predicted for a brown dwarf, M2 = 0.054+/-0.010 Msol and R2 = 0.089+/-0.005 Rsol. Our results do not agree with the recent determination of Vuckovic et al. 2008 based on a K2 estimate from line-profile asymmetries.

arXiv commentAccepted by MNRAS

References in corpus (3)

• New VI photometry of the sdOB binary AA Dor and an improved photometric model
• The rotational velocity of the sdOB primary of the eclipsing binary system LB 3459 (AA Dor)
• FUSE spectroscopy of sdOB primary of the post common-envelope binary LB 3459 (AA Dor)

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