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Title:
Spectroscopy of the growing circumstellar disk in the delta Scorpii Be binary
Authors:
Miroshnichenko, A. S.; Bjorkman, K. S.; Morrison, N. D.; Wisniewski, J. P.; Manset, N.; Levato, H.; Grosso, M.; Pollmann, E.; Buil, C.; Knauth, D. C.
Affiliation:
AA(Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA; Pulkovo Observatory, Saint-Petersburg 196140, Russia), AB(Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA), AC(Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA), AD(Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA), AE(CFHT Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA), AF(Complejo Astronómico El Leoncito (CASLEO), Casilla de Correo 467, 5400 San Juan, Argentina), AG(Complejo Astronómico El Leoncito (CASLEO), Casilla de Correo 467, 5400 San Juan, Argentina), AH(Charlottenburgerstrasse 26c, 511377 Leverkusen, Germany), AI(6 place Clémence Isaure, 31320 Castanet-Toloson, France), AJ(Department of Physics and Astronomy, John Hopkins University, 3400 N. Charles Str., Baltimore, MD 21218, USA)
Publication:
Astronomy and Astrophysics, v.408, p.305-311 (2003) (A&A Homepage)
Publication Date:
09/2003
Origin:
A&A
Astronomy Keywords:
techniques: spectroscopic, stars: circumstellar matter, stars: individual: delta Scorpii, stars: binaries: spectroscopic, stars: Be stars
DOI:
10.1051/0004-6361:20030965
Bibliographic Code:
2003A&A...408..305M

Abstract

We present the results of a spectroscopic monitoring program of the binary system delta Scorpii, whose primary became a Be star after the last periastron encounter in the Summer of 2000. The observations cover a period of 2 years (March 2001-June 2003) and are a continuation of our previous campaign reported in Miroshnichenko et al. (\cite{metal}). We found that the emission-line spectrum was gradually strengthening over the whole monitoring period. Several short-term increases of the line emission, possibly due to outbursts of matter ejected from the stellar surface, were detected. The outbursts seem to be responsible for the brightness fadings, seen afterwards. We attempt to explain the overall observed line and continuum behaviour in terms of a circumstellar disk, growing in density and size. The disk is most likely Keplerian with an outer radius of ~10 Rstar and a mean expansion speed of ~ 0.4 km s-1.

Tables 1-2 are also available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/408/305}

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