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We present a seismic study of the β Cephei star θ Ophiuchi. Our analysis is based on the observation of one radial mode, one rotationally split  ℓ= 1  triplet and three components of a rotationally split  ℓ= 2  quintuplet for which the  m  values were well identified by spectroscopy. We identify the radial mode as fundamental, the triplet as  p  1  and the quintuplet as  g  1 . Our non‐local thermodynamic equilibrium abundance analysis results in a metallicity and CNO abundances in full agreement with the most recent updated solar values. With   X ∈[0.71, 0.7211]  and   Z ∈[0.009, 0.015] , and using the Asplund et al. mixture but with a Ne abundance about 0.3 dex larger, the matching of the three independent modes enables us to deduce constrained ranges for the mass  ( M = 8.2 ± 0.3 M ⊙ )  and central hydrogen abundance  ( X  c = 0.38 ± 0.02)  of θ Oph and to prove the occurrence of core overshooting  (α ov = 0.44 ± 0.07) . We also derive an equatorial rotation velocity of  29 ± 7 km s −1  . Moreover, we show that the observed non‐equidistance of the  ℓ= 1  triplet can be reproduced by the second‐order effects of rotation. Finally, we show that the observed rotational splitting of two modes cannot rule out a rigid rotation model.

An asteroseismic study of the β Cephei star θ Ophiuchi: constraints on global stellar parameters and core overshooting