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In order to make astroseismology a powerful tool to explore stellarinteriors, different numerical codes should give the same oscillationfrequencies for the same input physics. This work is devoted to test, compareand, if needed, optimize the seismic codes used to calculate theeigenfrequencies to be finally compared with observations. The oscillationcodes of nine research groups in the field have been used in this study. Thesame physics has been imposed for all the codes in order to isolate thenon-physical dependence of any possible difference. Two equilibrium models withdifferent grids, 2172 and 4042 mesh points, have been used, and the lattermodel includes an explicit modelling of semiconvection just outside theconvective core. Comparing the results for these two models illustrates theeffect of the number of mesh points and their distribution in particularlycritical parts of the model, such as the steep composition gradient outside theconvective core. A comprehensive study of the frequency differences found forthe different codes is given as well. These differences are mainly due to theuse of different numerical integration schemes. The use of a second-orderintegration scheme plus a Richardson extrapolation provides similar results toa fourth-order integration scheme. The proper numerical description of theBrunt-Vaisala frequency in the equilibrium model is also critical for somemodes. An unexpected result of this study is the high sensitivity of thefrequency differences to the inconsistent use of values of the gravitationalconstant (G) in the oscillation codes, within the range of the experimentallydetermined ones, which differ from the value used to compute the equilibriummodel.

Inter-comparison of the g-, f- and p-modes calculated using different oscillation codes for a given stellar model