Complexity of magnetic fields on red dwarfs | Astronomy & Astrophysics (A&A)

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Volume 629 (September 2019)

A&A, 629 (2019) A83

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Table 2

Summary of iterative χ² minimizationprocedure used in this paper.

Species	Used	Assumed	Retrieved	Range, step	Probed atmosphere features
	stokes
Ti I 8380 Å	I	B = 0	T_phot(Ti)	2000–4000 K, 100 K	An average photosphere
					with the highest temperature

Mol1	I	T_phot(Ti)	T_mag	2000–4000 K, 100 K	Starspots: TiO and FeH lines
		T_mag ≤T_phot	f_I	0.0–1.0, 0.1	were fitted separately
					(form at different heights)

Mol2	I	T_phot(Ti)	T_mag	2000–4000 K, 100 K	Magnetic network
		T_mag ≤T_phot	f_I	0.0–1.0, 0.1

Atoms	I, V	T_phot = T_mag	B	0–7000 G, 100 G	Magnetic network
			f_V	0.0–0.2, 0.01

Mol1	I, V	T_phot(Ti)	B	0–7000 G, 100 G	Starspots
		T_mag	f_V	0.0–0.2, 0.01
		f_I

Mol2	I	T_phot(Ti)	B	0–7000 G, 100 G	Magnetic network
		T_mag			The Stokes V signals
		f_I			are too weak and not used

Notes. The sets of spectral features (atoms, mol1, mol2) are described in Sect. 4.1. The results are presented in Table 3 and shown in Fig. 4.

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