Hostname: page-component-8448b6f56d-42gr6 Total loading time: 0 Render date: 2024-04-20T11:18:25.429Z Has data issue: false hasContentIssue false

The unusual binary HD 83058 in the region of the Scorpius-Centaurus OB association

Published online by Cambridge University Press:  07 August 2014

M. A. Pogodin
Affiliation:
Pulkovo Observatory of Russian Academy of Sciences, Pulkovskoe shosse 65/1, 196135, Saint Petersburg, Russia email: pogodin@gao.spb.ru
N. A. Drake
Affiliation:
Saint Petersburg State University, Universitetski pr. 28, Petrodvorets, 198504, Saint Petersburg, Russia, email: drake@on.br Observatório Nacional/MCTI, Rua General José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: claudio@on.br
E. G. Jilinski
Affiliation:
Pulkovo Observatory of Russian Academy of Sciences, Pulkovskoe shosse 65/1, 196135, Saint Petersburg, Russia email: pogodin@gao.spb.ru Observatório Nacional/MCTI, Rua General José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: claudio@on.br Instituto de Física, Universidade do Estado do Rio de Janeiro (UERJ), Rua São Francisco Xavier 524, Maracanã, 200550-900, Rio de Janeiro, Brazil, email: jilinski@on.br
C. B. Pereira
Affiliation:
Observatório Nacional/MCTI, Rua General José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: claudio@on.br
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the results of high-resolution spectroscopy of the binary system HD 83058 situated in the region of the Sco-Cen OB association. On the base of the radial-curve solution we have determined the elements of the orbit and determined the period P = 2.365102 days. We have disentangled the spectra of the two components of the system and derived the basic parameters of both components. We have shown that moving features in the Si iii line profiles seen in the spectra of the primary can be interpreted in the frame of the assumption of the rotation of local spot-like inhomogeneities on the stellar surface. We have also found that the lines in the spectrum of the secondary show another type of variability.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Hubeny, I. & Lanz, T. 1992, A&A, 262, 501Google Scholar
Jilinski, E., Ortega, V. G., Drake, N. A., & de la Reza, R. 2010, ApJ, 721, 469Google Scholar
Piskunov, N. E. 1992, Stellar Magnetism, 92Google Scholar
Telting, J. H., Schrijvers, C., Ilyin, I. V., et al. 2006, A&A, 452, 945Google Scholar