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| Paper: |
The Be Binary δ Scorpii and Its 2011
Periastron Passage |
| Volume: |
464, Circumstellar Dynamics at High Resolution |
| Page: |
187 |
| Authors: |
Miroshnichenko, A. S.; Manset, N.; Pasechnik, A. V.; Carciofi, A. C.; Rivinius, Th.; Štefl, 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. |
| Abstract: |
δ 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. |
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