Standing torsional Alfvén waves as the source of the rotational period variation in magnetic early-type stars

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Table 1.

Magnetic stars that show rotational period variations.

Object	HD	log T_eff	log L/L_⊙	B_pole	P_rot	T_baseline	dP_rot/dt	M_ini	τ	τ/τ_MS
		K		kG	d	yr	10⁻² s yr⁻¹	M_⊙	Myr
σ Ori E	37 479	4.361 ± 0.039 ^(a)	3.51 ± 0.21 ^(a)	$7 . 55_{- 0.25}^{+ 0.25}$ $7.55^{+0.25}_{-0.25}$ ^(b)	1.191 ^(a)	43 (1974–2017) ^(c)	9.71 ± 0.09 ^(c)	8.5	4.33	0.1
V901 Ori	37 776	4.342 ± 0.019 ^(a)	3.30 ± 0.15 ^(a)	$6 . 1_{- 0.7}^{+ 0.7}$ $6.1^{+0.7}_{-0.7}$ ^(a)	1.539 ^(a)	36 (1977–2013) ^(d)	35.3 ± 0.9 ^(c)	7.5	0.00	0.0
V913 Sco	142 990	4.255 ± 0.012 ^(a)	2.93 ± 0.13 ^(a)	$4 . 7_{- 0.4}^{+ 0.4}$ $4.7^{+0.4}_{-0.4}$ ^(a)	0.979 ^(a)	39 (1976–2015) ^(e)	−58 ± 1 ^(e)	5.5	27.6	0.3
56 Ari	19 832	4.093 ± 0.013 ^(a)	2.08 ± 0.16 ^(a)	$2 . 7_{- 0.3}^{+ 0.6}$ $2.7^{+0.6}_{-0.3}$ ^(a)	0.728 ^(a)	48 (1952–2001) ^(f)	2.25 ^(f)	3.2	196	0.6
V343 Pup	60 431	4.114 ± 0.01 ^(g)	2.00 ± 0.032 ^(g)	–	0.476 ^(g)	35 (1986–2021) ^(g)	0.74 ± 0.05 ^(g)	3.2	45.1	0.1
CU Vir	124 224	4.089 ± 0.003 ^(a)	1.93 ± 0.01 ^(a)	$4 . 0_{- 0.2}^{+ 0.2}$ $4.0^{+0.2}_{-0.2}$ ^(h)	0.521 ^(a)	67 (1949–2016) ^(c)	8.817 ± 12 ^(c)	3.0	54.5	0.1
13 And	220 885	4.03 ± 0.05 ⁽ⁱ⁾	1.87 ± 0.2 ⁽ⁱ⁾	–	1.479 ^(d)	23 (1990–2013) ^(d)	−63.4 ^(d)	2.7	306	0.6
V473 Tau	30 466	4.045 ± 0.011 ^(j)	1.64 ± 0.15 ^(j)	–	1.407 ^(j)	47 (1963–2010) ^(j)	−11 ± 3 ^(j)	2.5	71.9	0.1
BS Cir	125 630	3.966 ± 0.014 ^(k)	1.72 ± 0.10 ^(k)	–	2.204 ^(c)	39 (1975–2014) ^(c)	17.0 ± 1.3 ^(c)	2.5	493	0.8
CS Vir	125 248	3.992 ± 0.013 ^(a)	1.50 ± 0.08 ^(a)	$9 . 0_{- 1.3}^{+ 1.1}$ $9.0^{+1.1}_{-1.3}$ ^(a)	9.300 ^(a)	83 (1928–2011) ^(l)	66 ± 8 ^(l)	2.2	184	0.2

Notes. Columns: T_eff, L, and B_pole are the effective temperature, the luminosity, and the magnetic field strength at the magnetic pole, respectively. T_baseline is the baseline duration of the observations for rotational periods. M_ini, τ, and τ/τ_MS are the initial mass, the age, and the main-sequence fractional age, respectively, which were estimated theoretically via fitting to the location in the HR diagram.

^(a)

Shultz et al. (2022)

^(b)

Oksala et al. (2015)

^(c)

Mikulášek (2016)

^(d)

Pyper & Adelman (2020)

^(e)

Shultz et al. (2019a)

^(f)

Adelman et al. (2001)

^(g)

Mikulášek et al. (2022)

^(h)

Kochukhov et al. (2014)

⁽ⁱ⁾

SIMBAD photometry

^(j)

Ozuyar & Stevens (2018)

^(k)

Kochukhov & Bagnulo (2006)

^(l)

Ozuyar et al. (2018)

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