The Be binary delta Scorpii and Its 2011 periastron passage

Miroshnichenko, A.S.; Manset, N.; Pasechnik, A.V.; Carciofi, A.C.; Rivinius, T.; Stefl, S.; Ribeiro, J.M.; Garrel, T.; Knapen, J.H.; Buil, C.; Heathcote, B.; Pollmann, E.; Thizy, O.; Eversberg, T.; Reinecke, N.; Martin, J.; Okazaki, A.T.; Gandet, T.L.; Gvaramadze, V.V.; Zharikov, S.V.

Авторы: Miroshnichenko A.S., Manset N., Pasechnik A.V., Carciofi A.C., Rivinius Th, Stefl S., Ribeiro J.M.Fernando A, Garrel T., Knapen J.H., Buil C., Heathcote B., Pollmann E., Thizy O., Eversberg T., Reinecke N., Martin J., Okazaki A.T., Gandet T.L., Gvaramadze V.V., Zharikov S.V.
Сборник: Circumstellar Dynamics at High Resolution. Proceedings of a Joint ESP/Brazilian Workshop
Серия: ASP Conference Proceedings
Том: 464
Год издания: 2012
Место издания: Astronomical Society of the Pacific San Francisco
Первая страница: 187
Последняя страница: 194
Аннотация: Delta Scorpii is an unusual Be binary system. The binarity was discovered by interferometry in the 1970's and only confirmed by radial velocity measurements during the periastron passage in September 2000, when the primary component became a Be star. The components brightness and mass suggest that both are normal B-type stars. However, the large orbital eccentricity (e=0.94) is highly uncommon, as most such Be binaries have circular orbits. The orbital period, only recently constrained by interferometry at 10.81 years, needed confirmation from spectroscopy during the last periastron passage in July 2011. The periastron observing campaign that involved professionals and amateurs resulted in obtaining several hundreds of spectra during the period of a large radial velocity change compared to only thirty obtained in 2000. Along with a determination of the orbital period accurate to 3-4 days, the radial velocity curve was found to be more complicated than one expected from just a binary system. I will briefly review the primary's disk development followed by a discussion of the recent observations. Implications for the system properties and ideas for future observations will be presented.
Добавил в систему: Гварамадзе Василий Васильевич

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