SIMBAD references

2012MNRAS.427..483B - Mon. Not. R. Astron. Soc., 427, 483-493 (2012/November-3)

Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field.

BRIQUET M., NEINER C., AERTS C., MOREL T., MATHIS S., REESE D.R., LEHMANN H., COSTERO R., ECHEVARRIA J., HANDLER G., KAMBE E., HIRATA R., MASUDA S., WRIGHT D., YANG S., PINTADO O., MKRTICHIAN D., LEE B.-C., HAN I., BRUCH A., DE CAT P., UYTTERHOEVEN K., LEFEVER K., VANAUTGAERDEN J., DE BATZ B., FREMAT Y., HENRICHS H., GEERS V.C., MARTAYAN C., HUBERT A.M., THIZY O. and TIJANI A.

Abstract (from CDS):

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= 7.14846d–1) and by rotational modulation (Prot= 3.638833d). Two non-radial low-amplitude modes (f2 = 7.75603d–1 and f3= 6.82308d–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 f3are 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. 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.

F.R.S. – FNRS Postdoctoral Researcher, Belgium.

Guest investigator, Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada.


Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS

Journal keyword(s): stars: early-type - stars: individual: V2052 Oph - stars: interiors - stars: magnetic field - starspots

Simbad objects: 17

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2019.10.20-17:58:18

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