  The binary star delta 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 +/- 1 mas formed around the primary
in 2000. By 2006/2007 the size of this region grew to an estimated > 4 mas.
  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 +/- 7 Msun and Mb = 8.0 +/- 3.6
Msun. The dynamical parallax is estimated to be 7.03 +/- 0.15 mas, which is in
good agreement with the revised HIPPARCOS parallax.
