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Title:
Spectroscopic observations of the δ Scorpii binary during its recent periastron passage
Authors:
Miroshnichenko, A. S.; Fabregat, J.; Bjorkman, K. S.; Knauth, D. C.; Morrison, N. D.; Tarasov, A. E.; Reig, P.; Negueruela, I.; Blay, P.
Affiliation:
AA(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA; Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 196140 Saint-Petersburg, Russia), AB(Universidad de Valencia, Departamento de Astronomía, 46100 Burjassot, Valencia, Spain), AC(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA), AD(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA), AE(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA), AF(Crimean Astrophysical Observatory and Isaac Newton Institute of Chile, Crimean Branch, Nauchny, Crimea, 98409, Ukraine), AG(Foundation for Research and Technology-Hellas, 711 10 Heraklion, Crete, Greece; Physics Department, University of Crete, 710 33 Heraklion, Crete, Greece), AH(Observatoire de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France), AI(Universidad de Valencia, Departamento de Astronomía, 46100 Burjassot, Valencia, Spain)
Publication:
Astronomy and Astrophysics, v.377, p.485-495 (2001) (A&A Homepage)
Publication Date:
10/2001
Origin:
A&A
Astronomy Keywords:
STARS: EMISSION-LINE, BE, BINARIES: CLOSE, INDIVIDUAL: DELTA SCO, TECHNIQUES: SPECTROSCOPIC
DOI:
10.1051/0004-6361:20010911
Bibliographic Code:
2001A&A...377..485M

Abstract

The bright star delta 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 delta 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. This paper is partly based on observations obtained at the European Southern Observatory and the South African Astronomical Observatory.
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