Magnetic cycles at different ages of stars | Astronomy & Astrophysics (A&A)

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Table 1

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

Star	Sp. type	P_rot	P_cyc,(range)	lt^c	P_cyc, Baliunas et al. (1995)
		(days)	(years)		(years)

simple cycles

HD 3651	K0V^a	44^b	11.6(9.57–13.7)-lt	yes	13.8 ± 0.4
HD 4628	K2.5V^a	41.6	8.94(8.30–9.5)	no	8.37 ± 0.08
HD 10476	K1V^a	33.7	9.8(9.01–9.85)	no	9.6 ± 0.1
HD 16160	K3V^a	57	12.1	no	13.2 ± 0.2
HD 26965	K1V^a	43^b	10.0(9.57–10.5)	no	10.1 ± 0.1
HD 32147	K3+V^a	39.3	10.6(9.85–11.3), lt	yes	11.1 ± 0.2
HD 81809	G5V^a	39.3	8.69(8.10–9.28)	no	8.17 ± 0.08
HD 103095	K1V^a	36.5	6.95(6.9–7.0), lt	yes	7.30 ± 0.08
HD 160346	K2.5V^a	35.3	7.35(7.2–7.5), lt	yes	7.00 ± 0.08
HD 166620	K2V^c	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	G2V^a	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	G3V^a	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	F9.5V^a	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	K2.5V^a	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	K0V^a	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+V^a	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	K0V^a	18.9	11.4(9–13.8), 5.17, lt	yes	5.1 ± 0.1
HD 165341B	K6V	–	–		Var
HD 190406	G0V^a	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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