Surface-effect corrections for solar-like oscillations using 3D hydrodynamical simulations - I. Adiabatic oscillations

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Table 2

Characteristics of UPM and PM.

Model	M^a	Age	α_MLT	R_PM	R_PM/R_UPM−1	Stage^b
	[M_⊙]	[Gyr]		[R_⊙]

A	1.01	4.61	1.65	1.00	2.08 × 10^-4	MS
B	1.37	1.36	1.69	1.45	1.44 × 10^-3	MS
C	1.47	2.30	1.68	2.01	1.23 × 10^-3	MS
D	1.26	2.60	1.69	1.39	7.54 × 10^-4	MS
E	1.38	3.20	1.69	1.94	8.61 × 10^-4	MS
F	1.12	5.43	1.68	1.31	5.75 × 10^-4	MS
G	1.08	0.0209	1.66	0.967	2.21 × 10^-4	MS
H	1.14	6.93	1.70	1.77	6.15 × 10^-4	SG
I	1.73	1.76	1.65	3.83	1.65 × 10^-4	RG
J	3.76	0.213	1.61	18.2	2.16 × 10^-3	RG

Notes.

^(a)

The stellar masses for UPM and PM differ by at most a fraction ~10^-7.

^(b)

Evolutionary stage. MS, SG, and RG mean the main sequence, subgiant, and red giant stages, respectively.

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