Table 4.
Changes of the mean magnetic field and Fe abundance inferred in the two-component modelling caused by temperature variations.
| Star | Teff (K) | Change in Teff |
Magnetic spots |
||||
|---|---|---|---|---|---|---|---|
| ΔTeff (K) | Δ⟨B⟩I (G) | ΔεFe | ΔTspot (K) | Δ⟨B⟩I (G) | ΔεFe | ||
| HD 1835 | 5837 | +50 | −0.29 | 0.023 | +200 | 8.52 | 0.016 |
| −50 | 0.77 | −0.023 | −200 | −11.56 | −0.019 | ||
| HD 9986 | 5805 | +50 | 20.53 | 0.021 | +200 | −7.64 | 0.006 |
| −50 | −7.42 | −0.021 | −200 | 41.15 | 0.041 | ||
| HD 22049 | 5146 | +50 | 8.46 | 0.015 | +200 | −1.76 | 0.008 |
| −50 | −7.66 | −0.014 | −200 | −1.02 | −0.006 | ||
| HD 75732 | 5235 | +50 | 0.50 | 0.016 | +200 | −24.60 | 0.070 |
| −50 | −1.13 | −0.016 | −200 | −13.90 | 0.000 | ||
Notes. The left half of the table corresponds to a change in Teff by ±50 K. The right half shows the impact of the assumption that the magnetically active regions correlate with temperature inhomogeneities on the stellar surface by considering a different temperature in the magnetic and non-magnetic areas.
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