What causes the large extensions of red supergiant atmospheres? - Comparisons of interferometric observations with 1D hydrostatic, 3D convection, and 1D pulsating model atmospheres

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Table 5

RHD simulations of red supergiant stars used in this work.

Model	Grid	M _pot	L	T _eff	R _⋆	log g
	[grid points]	[M_⊙]	[L_⊙]	[K]	[R_⊙]	[cgs]

st35gm03n07^a	235³	12	91 932±1400	3487±12	830.0±2.0	−0.335±0.002
st35gm03n13^b	235³	12	89 477±857	3430±8	846.0±1.1	−0.354±0.001
st36gm00n06	255³	6	23 994±269	3660±11	391.3±1.5	0.010±0.004
st36gm00n05^b	401³	6	24 233±535	3710±20	376.7±0.5	0.047±0.001

Notes.

^(a)

Used in Chiavassa et al. (2009; 2010b; 2011b).

^(b)

Chiavassa et al. (2011a).

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