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Table 1

All detected cycles in the MW stars; the first is the dominant cycle.

Star Sp. type Prot Pcyc,(range) ltc Pcyc, Baliunas et al. (1995)
(days) (years) (years)
simple cycles
HD 3651 K0Va 44b 11.6(9.57–13.7)-lt yes 13.8 ± 0.4
HD 4628 K2.5Va 41.6 8.94(8.30–9.5) no 8.37 ± 0.08
HD 10476 K1Va 33.7 9.8(9.01–9.85) no 9.6 ± 0.1
HD 16160 K3Va 57 12.1 no 13.2 ± 0.2
HD 26965 K1Va 43b 10.0(9.57–10.5) no 10.1 ± 0.1
HD 32147 K3+Va 39.3 10.6(9.85–11.3), lt yes 11.1 ± 0.2
HD 81809 G5Va 39.3 8.69(8.10–9.28) no 8.17 ± 0.08
HD 103095 K1Va 36.5 6.95(6.9–7.0), lt yes 7.30 ± 0.08
HD 160346 K2.5Va 35.3 7.35(7.2–7.5), lt yes 7.00 ± 0.08
HD 166620 K2Vc 41.5 13.6(9.6–17.6) no 15.8 ± 0.3
HD 201091 K5V 37.1 6.95(6.7–7.2), lt yes 7.3 ± 0.1
HD 219834B K2V 34.0 9.29(9.01–9.57) no 10.0 ± 0.2
Sun G2V 27.275 11(9–14), 3.65(3.3–4.0)d yes
complex cycles
HD 1835 G2Va 7.84 7.6(7.3–7.9), 2.4(2.50–2.28), 3.97(4.85–3.09), lt yes 9.1 ± 0.3
HD 20630 G5V 9.08 5.32(5.36–5.27) no 5.6 ± 0.1
HD 76151 G3Va 15.2 5.32(6.07–4.56), lt yes 2.52 ± 0.02
HD 78366 G0V 9.7 13.45(12.6–14.3)-lt, 4.0(3.85–4.15) yes 12.2 ±0.4, 5.9 ± 0.1
HD 95735 M2V 54 3.90(3.75-4.04), 12.7(10.3-15.0)-lt yes
HD 100180 F9.5Va 14.6 13.2(16.6–9.85), 3.63 no 3.56 ± 0.04, 12.9 ± 0.5
HD 114710 G0V 12.9 16.6(17.6–13.7–18.6), 7.7(7.2–8.2), 5.25(5.1–5.4) no 16.6 ± 0.6, 9.6 ± 0.3
HD 115404 K2.5Va 18.8 10.8(9.57–12.1), 5.08(5.83–4.33), 3.4(3.96–2.84) lt yes 12.4 ± 0.4
HD 131156A G8V 6.25 3.7(3.6–3.8), 12, lt yes
HD 131156B K4V 11.05 4.2(4.64–3.76), 2.28, lt yes
HD 149661 K0Va 21.3 4.0, 6.2(5.6–6.8), 12.25(11.3–13.2)-lt yes 17.4 ± 0.7, 4.00 ± 0.04
HD 152391 G8+Va 11.4 9.9(12.6–7.17), 2.8(2.5–3.1) no 10.9 ± 0.2
HD 156026 K5V 29.2 4.33(3.95–4.71), 8.1, lt(≈20) yes 21.0 ± 0.9
HD 165341A K0Va 18.9 11.4(9–13.8), 5.17, lt yes 5.1 ± 0.1
HD 165341B K6V – – Var
HD 190406 G0Va 15.5 15.8(15.0–17.6)-lt, 8.35(7.69–9.01), 4.65(4.44–4.86), 2.33, 3.01 yes 2.60 ± 0.02, 16.9 ± 0.8
HD 201092 K7V 34.1 13.4(10.1–16.6)-lt, 4.45(4.71–4.18), (2.07:) yes 11.7 ± 0.4

Notes. In the last column we list results from Baliunas et al. (1995) for comparison.

(a)

Spectral types are taken from Gray et al. (2003, 2006), otherwise from Baliunas et al. (1995);

(b)

period form Barnes et al. (2007);

(c)

lt: long-term trend in the data;

(d)

determined in the present paper.

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