Volume 377, Number 2, October II 2001
|Page(s)||485 - 495|
|Section||Interstellar and circumstellar matter|
|Published online||15 October 2001|
Spectroscopic observations of the δ Scorpii binary during its recent periastron passage*
Ritter Observatory, Dept. of Physics & Astronomy, University of Toledo, Toledo, OH 43606, USA
2 Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 196140 Saint-Petersburg, Russia
3 Universidad de Valencia, Departamento de Astronomía, 46100 Burjassot, Valencia, Spain
4 Crimean Astrophysical Observatory and Isaac Newton Institute of Chile, Crimean Branch, Nauchny, Crimea, 98409, Ukraine
5 Foundation for Research and Technology-Hellas, 711 10 Heraklion, Crete, Greece
6 Physics Department, University of Crete, 710 33 Heraklion, Crete, Greece
7 Observatoire de Strasbourg, 11 rue de lUniversité, 67000 Strasbourg, France
Corresponding author: A. S. Miroshnichenko, email@example.com
Accepted: 20 June 2001
The bright star δ Sco has been considered a typical B0-type object for many years. Spectra of the star published prior to 1990 showed no evidence of emission, but only of short-term line profile variations attributed to nonradial pulsations. Speckle interferometric observations show that δ Sco is a binary system with a highly-eccentric orbit and a period of ~10.6 years. Weak emission in the Hα line was detected in its spectrum for the first time during a periastron passage in 1990. Shortly before the next periastron passage in the summer of 2000, the binary entered a strong Hα emission and enhanced mass-loss phase. We monitored the spectroscopic development of the Be outburst from July 2000 through March 2001. In this paper we present results from our spectroscopy, refine elements of the binary orbit, and discuss possible mechanisms for the mass loss.
Key words: stars: emission-line, Be / binaries: close / stars: individual: δ Sco / techniques: spectroscopic
© ESO, 2001
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