Table 2
Statistical properties of photospheric micro-turbulence of the sample non-radial pulsators separated by the type of oscillations and of the classical Cepheids and red giants and supergiants divided into two mass-luminosity subgroups.
| SpT | Type of puls | # of stars | logTeff limits | log g limits | ℒ/ℒ⊙ limits | vmic limits (km s−1) | ρ, p (vmic, log g) | ρ, p (vmic, logTeff) | ![$\[\bar{v}_{\text {mic}}\]$](/articles/aa/full_html/2025/09/aa54907-25/aa54907-25-eq10.png) (km s−1) |
|---|---|---|---|---|---|---|---|---|---|
| β Cep | non-RPs | 14 | 4.44–4.30 | 4.15–3.50 | 2.673.45 | 0.0–14.0 | −0.78, 0.00a | +0.31, 0.28a | 6.1±4.0 |
| reference stars | non-var MS B | 112 | 4.43–4.22 | 4.40–3.20 | 2.67–3.45 | 0.0–14.0 | −0.26, 0.00 | +0.01, 0.89 | 5.6±3.6 |
| SPBs genuine | non-RPs | 41 | 4.34–4.04 | 4.30–3.05 | 1.59–3.28 | 2.0–7.0 | −0.07, 0.66 | −0.44, 0.00 | 3.9±1.7 |
| SPBs suspected | non-RPs | 13 | 4.13–4.00 | 3.60–2.83 | 1.79–2.79 | 2.0–6.6 | −0.36, 0.23 | +0.31, 0.30 | 3.7±1.3 |
| SPBs total | non-RPs | 54 | 4.34–4.00 | 4.30–2.83 | 1.59–3.28 | 2.0–7.0 | −0.14, 0.31 | −0.40, 0.00 | 3.8±1.6 |
| reference stars | non-var MS B | 158 | 4.51–4.00 | 4.57–3.04 | 1.72–3.27 | 0.0–13.0 | −0.16, 0.04 | +0.33, 0.00 | 3.9±3.2 |
| δ Scu | non-RPs | 44 | 3.97–3.80 | 3.40–4.32 | 0.42–1.58 | 1.2–4.1 | +0.09, 0.57 | non-mnt | 2.8±0.8 |
| γ Dor | non-RPs | 52 | 3.90–3.78 | 4.50–3.80 | 2.29–2.29 | 1.3–3.2 | −0.28, 0.04 | non-mnt | 3.1±0.4 |
| reference stars | non-var AF dws | 320 | 4.00–3.85 | 4.87–3.85 | 1.54–0.4 | 0.0–4.0 | −0.21, 0.23 | non-mnt | |
| Cepheids, total | RPs | 199 | 3.83–3.69 | 2.60–0.50 | 2.00–3.75 | 2.4–6.5 | +0.03, 0.68 | +0.04, 0.56 | 4.1±0.8 |
| Ceph Minit <9Msun | − | 164 | 3.83–3.69 | 2.60–1.18 | 2.00–3.08 | 2.4–6.3 | +0.09, 0.24 | +0.07, 0.34 | 4.0±0.8 |
| Ceph Minit >9Msun | − | 35 | 3.82–3.69 | 1.55–0.50 | 3.11–3.75 | 3.0–6.5 | −0.03, 0.88 | −0.08, 0.66 | 4.2±1.0 |
| RGs | var | 215 | 3.74–3.60 | 3.75–1.00 | 2.81–0.44 | 0.7–2.1 | −0.42, 2.58−10 | −0.24, 0.00 | 1.5±0.2 |
| RSGs | var | 7 | 3.60–3.59 | 1.00–0.30 | 3.45–2.81 | 1.1–1.6 | .... | .... | 1.3±0.2 |
Notes. ρ and p – the Spearman rang correlation coefficient and its significance. Significant, moderate to strong correlations are highlighted in bold. reference stars = sample non-variable stars of similar Teff, log g and spectral luminosity; SPBs = slowly pulsating B stars; SPBs suspected = stars which lie outside the instability strip for g mode oscillations but possess photometric and vmic properties similar to those of the genuine SPBs; RPs = radial pulsators; non-RPs = non-radial pulsators; var = variable stars; non-mnt = non-monotonic behaviour; “a” – due to lower statistics these results should be considered with caution.
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