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Title:
The 2011 Periastron Passage of the Be Binary delta Scorpii
Authors:
Miroshnichenko, A. S.; Pasechnik, A. V.; Manset, N.; Carciofi, A. C.; Rivinius, Th.; Stefl, S.; Gvaramadze, V. V.; Ribeiro, J.; Fernando, A.; Garrel, T.; Knapen, J. H.; Buil, C.; Heathcote, B.; Pollmann, E.; Mauclaire, B.; Thizy, O.; Martin, J.; Zharikov, S. V.; Okazaki, A. T.; Gandet, T. L.; Eversberg, T.; Reinecke, N.
Affiliation:
AA(Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27402-6170, USA), AB(Tuorla Observatory, Department of Physics and Astronomy, University of Turku, FI-21500 Pükkiö, Finland), AC(CFHT Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA), AD(Instituto de Astronomia, Geofísica e Ciéncias Atmosféricas, Universidade de São Paulo, Brazil), AE(European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile), AF(ESO/ALMA, Alonso de Córdova 3107, Vitacura, Santiago, Chile), AG(Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia ; Isaac Newton Institute of Chile, Moscow Branch, Universitetskij Pr. 13, Moscow 119992, Russia), AH(Observatorio do Instituto Geografico do Exercito, Lisboa, Portugal), AI(ATALAIA.org Group, Lisboa, Portugal), AJ(Observatoire de Juvignac, 19 avenue de Hameau du Golf F-34990, Juvignac, France), AK(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Spain), AL(Castanet Tolosan Observatory, 6 place Clèmence Isaure F-31320 Castanet Tolosan, France), AM(Barfold Observatory, Glenhope, Victoria 3444, Australia), AN(Emil-Nolde-Str. 12, D-51375, Leverkusen, Germany), AO(Observatoire du Val d'Arc, route de Peynier F-13530, Trets, France), AP(Shelyak Instruments, 1116 route de Chambery, F-38330, Saint-Ismier, France), AQ(Barber Research Observatory, Department of Physics and Astronomy, University of Illinois-Springfield, IL 62703, USA), AR(Instituto de Astronomia, Universidad Nacional Autónoma de Mexico, Apdo. Postal 877, Ensenada, 22800, Baja California, Mexico), AS(Faculty of Engineering, Hokkai-Gakuen University, Toyohira-ku, Sapporo 062-8605, Japan), AT(Lizard Hollow Observatory, P.O. Box 89175, Tucson, AZ 85752-9175, USA), AU(Schnörringen Telescope Science Institute, Waldbröl, Germany), AV(Fontainegraben 150, D-53123, Bonn, Germany)
Publication:
The Astrophysical Journal, Volume 766, Issue 2, article id. 119, 10 pp. (2013). (ApJ Homepage)
Publication Date:
04/2013
Origin:
IOP
Astronomy Keywords:
binaries: spectroscopic, stars: emission-line, Be, stars: individual: delta Sco
DOI:
10.1088/0004-637X/766/2/119
Bibliographic Code:
2013ApJ...766..119M

Abstract

We describe the results of the world-wide observing campaign of the highly eccentric Be binary system delta Scorpii 2011 periastron passage which involved professional and amateur astronomers. Our spectroscopic observations provided a precise measurement of the system orbital period at 10.8092 ± 0.0005 yr. Fitting of the He II 4686 Å line radial velocity curve determined the periastron passage time on 2011 July 3, UT 9:20 with a 0.9-day uncertainty. Both these results are in a very good agreement with recent findings from interferometry. We also derived new evolutionary masses of the binary components (13 and 8.2 M &sun;) and a new distance of 136 pc from the Sun, consistent with the HIPPARCOS parallax. The radial velocity and profile variations observed in the Halpha line near the 2011 periastron reflected the interaction of the secondary component and the circumstellar disk around the primary component. Using these data, we estimated a disk radius of 150 R &sun;. Our analysis of the radial velocity variations measured during the periastron passage time in 2000 and 2011 along with those measured during the 20th century, the high eccentricity of the system, and the presence of a bow shock-like structure around it suggest that delta Sco might be a runaway triple system. The third component should be external to the known binary and move on an elliptical orbit that is tilted by at least 40° with respect to the binary orbital plane for such a system to be stable and responsible for the observed long-term radial velocity variations.

This paper is partially based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique de France, and the University of Hawaii, the 2.2 m MPG telescope operated at ESO/La Silla under program IDs 086.A-9019 and 087.A-9005, the IAC80 telescope in the Spanish Observatorio del Teide of the Instituto de Astrofiísica de Canarias, and data from the ELODIE archive at the Observatoire de Haute-Provence.

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