Reference : An asteroseismic study of the β Cephei star θ Ophiuchi: spectroscopic results
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/126759
An asteroseismic study of the β Cephei star θ Ophiuchi: spectroscopic results
English
Briquet, Maryline mailto [Katholieke Universiteit Leuven - KUL > Instituut voor Sterrenkunde > > >]
Lefever, K. [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium]
Uytterhoeven, K. [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium]
Aerts, C. [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium]
1-Sep-2005
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
362
619-625
Yes (verified by ORBi)
International
0035-8711
Oxford
United Kingdom
[en] techniques: spectroscopic ; stars: early-type ; stars: individual: θ Oph ; stars: oscillations ; stars: variables: other
[en] We present the results of a detailed analysis of 121 ground-based high-resolution, high signal-to-noise ratio spectroscopic measurements spread over 3 yr for the β Cephei star θ Ophiuchi. We discovered θ Oph to be a triple system. In addition to the already known speckle B5 companion of the B2 primary, we showed the presence of a low-mass spectroscopic companion and we derived an orbital period of 56.71 d with an eccentricity of 0.1670. After removing the orbit we determined two frequencies for the primary in the residual radial velocities: f[SUB]1[/SUB]= 7.1160 cd[SUP]-1[/SUP] and f[SUB]2[/SUB]= 7.4676 cd[SUP]-1[/SUP]. We also found the presence of f[SUB]3[/SUB]= 7.3696 cd[SUP]-1[/SUP] by means of a two-dimensional frequency search across the SiIII 4567-Åprofiles. We identified the m-value of the main mode with frequency f[SUB]1[/SUB] by taking into account the photometric identifications of the degrees l. By means of the moment method and the amplitude and phase variations across the line profile, we derived (l[SUB]1[/SUB], m[SUB]1[/SUB]) = (2, -1). This result allows us to fix the mode identifications of the whole quintuplet for which three components were detected in photometry. This is of particular use for our forthcoming seismic modelling of the primary. We also determined stellar parameters of the primary by non-local thermodynamic equilibrium hydrogen, helium and silicon line profile fitting and we obtained T[SUB]eff[/SUB]= 24000 K and logg= 4.1, which is consistent with photometrically determined values.
http://hdl.handle.net/2268/126759
10.1111/j.1365-2966.2005.09287.x
http://esoads.eso.org/abs/2005MNRAS.362..619B
http://de.arxiv.org/abs/astro-ph/0506643

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