Extensive spectroscopic and photometric study of HD 25558, a long orbital-period binary with two SPB components. Issue Volume 9:Issue S301(2013) (18th February 2014)

• Record Type: Journal Article
• Authors: Sódor, Á.; De Cat, P.; Wright, D. J.; Neiner, C.; Briquet, M.; Dukes, R. J.; Fekel, F. C.; Henry, G. W.; Williamson, M. H.; Muterspaugh, M. W.; Brunsden, E.; Pollard, K. R.; Cottrell, P. L.; Maisonneuve, F.; Kilmartin, P. M.; Matthews, J. M.; Kallinger, T.; Beck, P. G.; Kambe, E.; Engelbrecht, C. A.; Czanik, R. J.; Yang, S.; Hashimoto, O.; Honda, S.; Fu, J.-N.; Castanheira, B.; Lehmann, H.; Behara, N.; Van Winckel, H.; Scaringi, S.; Menu, J.; Lobel, A.; Lampens, P.; Mathias, P.;
• Is Part Of: Proceedings of the International Astronomical Union. Volume 9:Issue S301(2013)
• Page Start: 491
• Page End: 492
• Publication Date: 2014-02-18
• Subjects: line: profiles, -- stars: binaries: general, -- stars: oscillations (including pulsations), -- stars: rotation, -- stars: variables: other; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921313015202
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: We carried out an extensive photometric and spectroscopic investigation of the SPB binary, HD 25558 (see Fig. 1 for the time and geographic distribution of the observations). The ~2000 spectra obtained at 13 observatories during 5 observing seasons, the ground-based multi-colour light curves and the photometric data from the MOST satellite revealed that this object is a double-lined spectroscopic binary with a very long orbital period of about 9 years. We determined the physical parameters of the components, and have found that both lie within the SPB instability strip. Accordingly, both components show line-profile variations consistent with stellar pulsations. Altogether, 11 independent frequencies and one harmonic frequency were identified in the data. The observational data do not allow the inference of a reliable orbital solution, thus, disentangling cannot be performed on the spectra. Since the lines of the two components are never completely separated, the analysis is very complicated. Nevertheless, pixel-by-pixel variability analysis of the cross-correlated line profiles was successful, and we were able to attribute all the frequencies to the primary or secondary component. Spectroscopic and photometric mode-identification was also performed for several of these frequencies of both binary components. The spectroscopic mode-identification results suggest that the inclination and rotation of the two components are rather different. While the primary is a slow rotator with ~6 d rotation period, seen at ~60° inclination, the secondary rotates fast with ~1.2 d rotation period, and is seen at ~20° inclination. Our spectropolarimetric measurements revealed that the secondary component has a magnetic field with at least a few hundred Gauss strength, while no magnetic field was detected in the primary. The detailed analysis and results of this study will be published elsewhere.