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Title:
A new determination of the orbit and masses of the Be binary system δ Scorpii
Authors:
Tango, W. J.; Davis, J.; Jacob, A. P.; Mendez, A.; North, J. R.; O'Byrne, J. W.; Seneta, E. B.; Tuthill, P. G.
Affiliation:
AA(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AB(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AC(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AD(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AE(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AF(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AG(Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE), AH(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 396, Issue 2, pp. 842-848. (MNRAS Homepage)
Publication Date:
06/2009
Origin:
MNRAS
Astronomy Keywords:
techniques: interferometric , binaries: spectroscopic , binaries: visual , stars: fundamental parameters , stars: individual: δ Sco , stars: individual: HR 5953
DOI:
10.1111/j.1365-2966.2009.14272.x
Bibliographic Code:
2009MNRAS.396..842T

Abstract

The binary star δ Sco (HD143275) underwent remarkable brightening in the visible in 2000, and continues to be irregularly variable. The system was observed with the Sydney University Stellar Interferometer (SUSI) in 1999, 2000, 2001, 2006 and 2007. The 1999 observations were consistent with predictions based on the previously published orbital elements. The subsequent observations can only be explained by assuming that an optically bright emission region with an angular size of >~2 +/- 1mas formed around the primary in 2000. By 2006/2007 the size of this region grew to an estimated >~4mas.

We have determined a consistent set of orbital elements by simultaneously fitting all the published interferometric and spectroscopic data as well as the SUSI data reported here. The resulting elements and the brightness ratio for the system measured prior to the outburst in 2000 have been used to estimate the masses of the components. We find MA = 15 +/- 7Msolar and MB = 8.0 +/- 3.6Msolar. The dynamical parallax is estimated to be 7.03 +/- 0.15mas, which is in good agreement with the revised Hipparcos parallax.

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