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

TL;DR

This study analyzes spectral data of AA Doradus to accurately determine the mass ratio and orbital parameters, revealing the primary is less massive and the secondary is consistent with a brown dwarf, challenging previous estimates.

Contribution

It provides a refined measurement of the mass ratio and component masses of AA Doradus using spectral line analysis and eclipse modeling, correcting earlier assumptions.

Findings

Measured Vsini = 31.8 km/s for the sdOB star.

Derived mass ratio q = 0.213.

Secondary's mass and radius are consistent with a brown dwarf.

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.