Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field
| dc.contributor.author | Briquet, M. | |
| dc.contributor.author | Neiner, C. | |
| dc.contributor.author | Aerts, C. | |
| dc.contributor.author | Morel, T. | |
| dc.contributor.author | Mathis, S. | |
| dc.contributor.author | Reese, D.R. | |
| dc.contributor.author | Lehmann, H. | |
| dc.contributor.author | Costero, R. | |
| dc.contributor.author | Echevarria, J. | |
| dc.contributor.author | Handler, G. | |
| dc.contributor.author | Kambe, E. | |
| dc.contributor.author | Hirata, R. | |
| dc.contributor.author | Masuda, S. | |
| dc.contributor.author | Wright, D. | |
| dc.contributor.author | Yang, S. | |
| dc.contributor.author | Pintado, O. | |
| dc.contributor.author | Mkrtichian, D. | |
| dc.contributor.author | Lee, B.-C. | |
| dc.contributor.author | Han, I. | |
| dc.contributor.author | Bruch, A. | |
| dc.contributor.author | De Cat, P. | |
| dc.contributor.author | Uytterhoeven, K. | |
| dc.contributor.author | Lefever, K. | |
| dc.contributor.author | Vanautgaerden, J. | |
| dc.contributor.author | De Batz, B. | |
| dc.contributor.author | Fremat, Y. | |
| dc.contributor.author | Henrichs, H. | |
| dc.contributor.author | Geers, V.C. | |
| dc.contributor.author | Martayan, C. | |
| dc.contributor.author | Hubert, A.M. | |
| dc.contributor.author | Thizy, O. | |
| dc.contributor.author | Tijani, A. | |
| dc.date | 2012 | |
| dc.date.accessioned | 2016-03-29T10:07:36Z | |
| dc.date.available | 2016-03-29T10:07:36Z | |
| dc.identifier.uri | https://orfeo.belnet.be/handle/internal/3000 | |
| dc.description | We used extensive ground-based multisite and archival spectroscopy to derive observational constraints for a seismic modelling of the magnetic β Cep star V2052 Ophiuchi. The line-profile variability is dominated by a radial mode (f1 = 7.148 46 d−1) and by rotational modulation (Prot = 3.638 833 d). Two non-radial low-amplitude modes (f2 = 7.756 03 d−1 and f3 = 6.823 08 d−1) are also detected. The four periodicities that we found are the same as the ones discovered from a companion multisite photometric campaign and known in the literature. Using the photometric constraints on the degrees ℓ of the pulsation modes, we show that both f2 and f3 are prograde modes with (ℓ, m) = (4, 2) or (4, 3). These results allowed us to deduce ranges for the mass (M ∈ [8.2, 9.6] M⊙) and central hydrogen abundance (Xc ∈ [0.25, 0.32]) of V2052 Oph, to identify the radial orders n1 = 1, n2 = −3 and n3 = −2, and to derive an equatorial rotation velocity veq ∈ [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 (αov ∈ [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 β Cep star θ 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. | |
| dc.language | eng | |
| dc.title | Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field | |
| dc.type | Article | |
| dc.subject.frascati | Physical sciences | |
| dc.audience | Scientific | |
| dc.source.title | Monthly Notices of the Royal Astronomical Society | |
| dc.source.volume | 427 | |
| dc.source.issue | 1 | |
| dc.source.page | 483-493 | |
| Orfeo.peerreviewed | Yes | |
| dc.identifier.doi | 10.1111/j.1365-2966.2012.21933.x | |
| dc.identifier.scopus | 2-s2.0-84868596488 |
