Reference : Spectroscopic mode identification for the slowly pulsating B star HD 147394
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/132659
Spectroscopic mode identification for the slowly pulsating B star HD 147394
English
Briquet, Maryline mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique stellaire théorique et astérosismologie >]
Aerts, C. [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium]
Mathias, P. [Observatoire de la Côte d'Azur, Département Fresnel, UMR 6528, 06304 Nice Cedex 4, France]
Scuflaire, Richard mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Evol. et stabilité des étoiles et des amas d'étoiles (ESEA)]
Noels-Grötsch, Arlette mailto [Institut d'Astrophysique et de Géophysique de Liège, Université de Liège, allée du Six Août 17, 4000 Liège, Belgium]
1-Apr-2003
Astronomy and Astrophysics
EDP Sciences
401
281-288
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] line: profiles ; stars: early-type ; stars: oscillations ; stars: rotation ; stars: variables: general ; stars: individual: HD 147394
[en] We present ground-based high-resolution high S/N spectra of the slowly pulsating B star HD 147394. Two frequencies are clearly found in the moments of the Si II 4128-4130 doublet: f[SUB]1[/SUB]=0.8008 c d[SUP]-1[/SUP] and f[SUB]2[/SUB]=0.7813 c d[SUP]-1[/SUP]. The frequency f[SUB]1[/SUB] is also found in the HIPPARCOS data. A third frequency is also present in our spectroscopic data: f[SUB]3[/SUB]=0.7175 c d[SUP]-1[/SUP] or its aliases due to the time sampling. A mode identification is performed by means of a new version of the moment method optimized for multiperiodic signals. It points towards several equivalent solutions of non-axisymmetric l <=3 for all three modes. We have too limited information to perform seismic modelling at this stage, but we do show that the different possibilities for the mode identifications are compatible with pulsational models for SPBs. Based on observations obtained with the spectrograph Aurélie attached to the 1.52-m telescope of the Observatoire de Haute-Provence, France.
Researchers ; Professionals
http://hdl.handle.net/2268/132659
10.1051/0004-6361:20030086
http://adsabs.harvard.edu/abs/2003A%26A...401..281B

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