Effects of magnetic fields on the center-to-limb variation in solar-type stars

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Table G.1

Fitting coefficients of the Claret-6 law – see Eq. (1) – for the nine MHD models. The data are given in ascending order of the field strength of the model.

I₁^(a)	c₁	c₂	c₃	c₄	c₅	c₆
1.213	1.142	−2.370	5.872	−7.263	4.669	−1.236
1.210	1.160	−2.441	6.049	−7.550	4.905	−1.312
1.205	1.166	−2.480	6.376	−8.331	5.636	−1.558
1.192	1.172	−2.426	6.568	−9.215	6.616	−1.913
1.162	1.130	−2.001	6.675	−11.480	9.452	−2.987
1.101	0.727	2.567	−5.766	2.799	2.063	−1.640
1.056	0.614	7.401	−25.214	33.159	−19.372	4.086
1.026	1.284	7.586	−36.588	58.799	−41.291	10.767
0.980	5.310	−17.384	22.456	−11.623	1.015	0.560

Notes. ^(a)/I₁ is the intensity at the disk center given in units of F/π, where F is the flux of the model in the Kepler passband.

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