Effective temperature determinations of late-type stars based on 3D non-LTE Balmer line formation

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Table 4

Differences between the effective temperatures of the benchmark stars inferred from various models compared to those inferred fromthe 3D non-LTE model (see Figs. 7–9 for illustrations of the 3D non-LTE fits).

Star
	Hα	Hβ	Hγ	Hα	Hβ	Hγ	Hα	Hβ	Hγ	Hα	Hβ	Hγ	Hα	Hβ	Hγ
Sun	− 5	− 1	1	− 31	− 53	− 30	− 33	− 26	94	− 40	− 57	− 31	− 43	− 31	94
Procyon	− 21	4	0	− 29	− 120	− 9	− 29	3	86	− 38	− 120	− 10	− 37	1	85
HD 103095	55	33	19	− 45	− 107	− 125	− 18	− 1	34	− 10	− 80	− 106	21	30	58
HD 84937	− 77	− 2	− 1	− 20	25	26	− 23	157	189	− 133	21	23	− 129	153	187
HD 140283	− 61	0	− 1	− 51	56	34	− 5	213	188	− 150	53	30	− 81	212	185
HD 122563	− 51	23	4	102	88	70	93	132	154	− 45	81	68	− 29	127	154

Notes. A positive value indicates that a higher effective temperature is inferred from the various models than from the 3D non-LTE models.

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