Reference : Asteroseismology of the β Cephei star ν Eridani - III. Extended frequency analysis an...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/126765
Asteroseismology of the β Cephei star ν Eridani - III. Extended frequency analysis and mode identification
English
De Ridder, J. [Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium]
Telting, J. H. [Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de La Palma, Spain]
Balona, L. A. [South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa]
Handler, G. [Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria]
Briquet, Maryline mailto [Katholieke Universiteit Leuven - KUL > Instituut voor Sterrenkunde > > >]
Daszyńska-Daszkiewicz, J. [Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium; Astronomical Institute of Wrocław University, ul. Kopernika 11, 51-622 Wrocław, Poland]
Lefever, K. [Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium]
Korn, A. J. [Department of Astronomy and Space Physics, Uppsala Astronomical Observatory, Box 515, SE-75120 Uppsala, Sweden]
Heiter, U. [Department of Astronomy and Space Physics, Uppsala Astronomical Observatory, Box 515, SE-75120 Uppsala, Sweden]
Aerts, C. [Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium]
1-Jun-2004
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
351
324-332
Yes (verified by ORBi)
International
0035-8711
Oxford
United Kingdom
[en] techniques: photometric ; techniques: spectroscopic ; stars: early-type ; stars: individual: ν Eridani ; stars: oscillations ; stars: variables: other
[en] Using the large photometric and spectroscopic data sets of the ν Eridani multisite campaign given in our two recent papers (Aerts et al. and Handler et al.), we present an extended frequency analysis and a photometric mode identification. For the extended frequency analysis, we used an improved radial velocity time series, the second-moment time series and the line profiles themselves. In the radial velocity time series, we can now detect an additional pulsation frequency that was previously only found in photometric time series. We also report several new candidate pulsation frequencies. For seven frequencies, the photometric mode identification indicates that they belong to a radial mode and six dipole modes, and for three frequencies the degree l could not be unambiguously determined. We also placed ν Eri in the Hertzsprung-Russell diagram by determining T[SUB]eff[/SUB] using Geneva plus Strömgren photometric calibrations, spectral energy distribution fitting, by non-local thermodynamic equilibrium hydrogen, helium and silicon line profile fitting, and by determining log(L/L[SUB]solar[/SUB]) using the Hipparcos parallax and an Hβ calibration.
http://hdl.handle.net/2268/126765
10.1111/j.1365-2966.2004.07791.x
http://esoads.eso.org/abs/2004MNRAS.351..324D

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