Spectropolarimetric characterisation of exoplanet host stars in preparation of the Ariel mission - II. The magnetised wind environment of TOI-1860, DS Tuc A, and HD 63433

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Volume 705 (January 2026)

A&A, 705 (2026) A40

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Table 3

Properties of the large-scale magnetic field and wind of the studied stars.

Star	⟨\|B_V\|⟩	\|B_V,max\|	$⟨ B_{V}^{2} ⟩$ $\[\langle\mathrm{B}_{\mathrm{V}}^{2}\rangle\]$	f_pol	f_tor	f_dip	f_quad	f_oct	f_ℓ=4	f_axi	f_axi,pol	f_axi,tor	$\dot{M}$ $\[\dot{\text{M}}\]$	$\dot{J}$ $\[\dot{\text{J}}\]$
	(G)	(G)	(G²)	(%)	(%)	(%)	(%)	(%)	(%)	(%)	(%)	(%)	(M_⊙/yr)	(erg)
TOI-1860	37	103	1.8 × 10³	28	72	28	13	26	20	73	11	98	1.5 × 10⁻¹³	1.4 × 10³¹
DS Tuc A	64	160	4.9 × 10³	64	36	67	12	9	5	76	63	98	4.4 × 10⁻¹³	1.2 × 10³²
HD 63433 (2023)	24	54	0.7 × 10³	46	54	30	25	15	10	66	38	90	1.1 × 10⁻¹³	4.9 × 10³⁰
HD 63433 (2024)	30	71	1.1 × 10³	47	53	7	23	20	36	51	7	91	1.4 × 10⁻¹³	4.5 × 10³⁰

Notes. The following quantities are listed: star name, mean unsigned large-scale magnetic strength, maximum unsigned large-scale magnetic strength, total reconstructed magnetic energy, poloidal and toroidal magnetic energies as a fraction of the total energy, dipolar, quadrupolar, and octupolar magnetic energy as a fraction of the poloidal energy, axisymmetric magnetic energy as a fraction of the total energy, poloidal axisymmetric energy as a fraction of the poloidal energy, toroidal axisymmetric energy as a fraction of the toroidal energy, mass loss rate, and angular momentum loss rate. The first row of HD 63433 refers to the 2023 ZDI reconstruction (Bellotti et al. 2024) while the second row to the 2024 reconstruction presented here.

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