000002739 001__ 2739
000002739 005__ 20160701171710.0
000002739 0247_ $$2DOI$$a10.1017/S1743921313015202
000002739 037__ $$aASTROimport-896
000002739 100__ $$aSódor, Á.
000002739 245__ $$aExtensive spectroscopic and photometric study of HD 25558, a long orbital-period binary with two SPB components
000002739 260__ $$c2014
000002739 520__ $$aWe carried out an extensive photometric and spectroscopic investigation of the SPB binary, HD 25558 (see Fig. 1 for the time and geographic distribution of the observations). The ~2000 spectra obtained at 13 observatories during 5 observing seasons, the ground-based multi-colour light curves and the photometric data from the MOST satellite revealed that this object is a double-lined spectroscopic binary with a very long orbital period of about 9 years. We determined the physical parameters of the components, and have found that both lie within the SPB instability strip. Accordingly, both components show line-profile variations consistent with stellar pulsations. Altogether, 11 independent frequencies and one harmonic frequency were identified in the data. The observational data do not allow the inference of a reliable orbital solution, thus, disentangling cannot be performed on the spectra. Since the lines of the two components are never completely separated, the analysis is very complicated. Nevertheless, pixel-by-pixel variability analysis of the cross-correlated line profiles was successful, and we were able to attribute all the frequencies to the primary or secondary component. Spectroscopic and photometric mode-identification was also performed for several of these frequencies of both binary components. The spectroscopic mode-identification results suggest that the inclination and rotation of the two components are rather different. While the primary is a slow rotator with ~6 d rotation period, seen at ~60° inclination, the secondary rotates fast with ~1.2 d rotation period, and is seen at ~20° inclination. Our spectropolarimetric measurements revealed that the secondary component has a magnetic field with at least a few hundred Gauss strength, while no magnetic field was detected in the primary. The detailed analysis and results of this study will be published elsewhere. 
000002739 700__ $$a De Cat, P.
000002739 700__ $$a Wright, D. J.
000002739 700__ $$a Neiner, C.
000002739 700__ $$a Briquet, M.
000002739 700__ $$a Dukes, R. J.
000002739 700__ $$a Fekel, F. C.
000002739 700__ $$a Henry, G. W.
000002739 700__ $$a Williamson, M. H.
000002739 700__ $$a Muterspaugh, M. W.
000002739 700__ $$a Brunsden, E.
000002739 700__ $$a Pollard, K. R.
000002739 700__ $$a Cottrell, P. L.
000002739 700__ $$a Maisonneuve, F.
000002739 700__ $$a Kilmartin, P. M.
000002739 700__ $$a Matthews, J. M.
000002739 700__ $$a Kallinger, T.
000002739 700__ $$a Beck, P. G.
000002739 700__ $$a Kambe, E.
000002739 700__ $$a Engelbrecht, C. A.
000002739 700__ $$a Czanik, R. J.
000002739 700__ $$a Yang, S.
000002739 700__ $$a Hashimoto, O.
000002739 700__ $$a Honda, S.
000002739 700__ $$a Fu, J.-N.
000002739 700__ $$a Castanheira, B.
000002739 700__ $$a Lehmann, H.
000002739 700__ $$a Behara, N.
000002739 700__ $$a Van Winckel, H.
000002739 700__ $$a Scaringi, S.
000002739 700__ $$a Menu, J.
000002739 700__ $$a Lobel, A.
000002739 700__ $$a Lampens, P.
000002739 700__ $$a Mathias, P.
000002739 773__ $$c491-492$$pPrecision Asteroseismology$$v301$$y2014
000002739 85642 $$ahttp://esoads.eso.org/abs/2014IAUS..301..491S
000002739 905__ $$apublished in
000002739 980__ $$aNONREF