Table 4
Summary of input and best-fit values for the PIMMS code when running on the minimum required number of observations, equally spread across a single rotation period, of the simulated β Cep and SPB stars described in Sect. 3.3.
| β Cep model | SPB model | |||
|---|---|---|---|---|
| Parameter | Input | PIMMS | Input | PIMMS |
| vp,1 | 20.0000 | 20.0194 | 15.0000 | 14.1673 |
| φ1 | 0.0000 | 0.0005 | 0.2000 | 0.2004 |
| K1 | 0.0000 | 0.0005 | 0.0100 | 0.0129 |
| vp,2 | 0.5000 | 0.5074 | ||
| φ2 | 0.3000 | 0.3002 | ||
| K2 | 0.0100 | 0.0110 | ||
| vp,3 | 0.5000 | 0.5205 | ||
| φ3 | 0.7000 | 0.7091 | ||
| K3 | 0.1000 | 0.0926 | ||
| Bd | 583 | 581 | 583 | 589 |
Notes. The number of observations is 19 and 109 for the β Cep and SPB models respectively. The β Cep star has 3 pulsation modes, and spots on the magnetic poles, while the SPB has a single pulsation mode and off-pole spots. Both models have dipolar magnetic fields.
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