M. Briquet, C. Neiner, C. Aerts, T. Morel, S. Mathis, D. R. Reese, H. Lehmann, R. Costero, J. Echevarria, G. Handler, E. Kambe, R. Hirata, S. Masuda, D. Wright, S. Yang, O. Pintado, D. Mkrtichian, B. -C. Lee, I. Han, A. Bruch, P. De Cat, K. Uytterhoeven, K. Lefever, J. Vanautgaerden, B. de Batz, Y. Frémat, H. Henrichs, V. C. Geers, C. Martayan, A. M. Hubert, O. Thizy, A. Tijani
We used extensive ground-based multisite and archival spectroscopy to derive observational constraints for a seismic modelling of the magnetic beta Cep star V2052 Ophiuchi. The line-profile variability is dominated by a radial mode (f_1=7.14846 d^{-1}) and by rotational modulation (P_rot=3.638833 d). Two non-radial low-amplitude modes (f_2=7.75603 d^{-1} and f_3=6.82308 d^{-1}) are also detected. The four periodicities that we found are the same as the ones discovered from a companion multisite photometric campaign (Handler et al. 2012) and known in the literature. Using the photometric constraints on the degrees l of the pulsation modes, we show that both f_2 and f_3 are prograde modes with (l,m)=(4,2) or (4,3). These results allowed us to deduce ranges for the mass (M \in [8.2,9.6] M_o) and central hydrogen abundance (X_c \in [0.25,0.32]) of V2052 Oph, to identify the radial orders n_1=1, n_2=-3 and n_3=-2, and to derive an equatorial rotation velocity v_eq \in [71,75] km s^{-1}. The model parameters are in full agreement with the effective temperature and surface gravity deduced from spectroscopy. Only models with no or mild core overshooting (alpha_ov \in [0,0.15] local pressure scale heights) can account for the observed properties. Such a low overshooting is opposite to our previous modelling results for the non-magnetic beta Cep star theta Oph having very similar parameters, except for a slower surface rotation rate. We discuss whether this result can be explained by the presence of a magnetic field in V2052 Oph that inhibits mixing in its interior.
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http://arxiv.org/abs/1208.4250
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