Three-dimensional simulations of near-surface convection in main-sequence stars - I. Overall structure

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Table 1

Stellar parameters, bolometric intensities, and rms velocities.

Simulation	log g^a	T_eff [K]	⟨I⟩/⟨I⟩_G2V^b	σ_I^c [%]	υ_z,rms(z) [km s^-1]
					z = z₀^d	z = z₂^e

F3V	4.301	6893.2 ±6.4	1.98	20.3	5.1	3.5
G2V	4.438	5764.4 ±7.4	1.00	15.7	2.0	1.2
K0V	4.609	4855.6 ±5.5	0.500	8.04	1.1	0.72
K5V	4.699	4367.9 ±2.0	0.322	6.90	0.99	0.57
M0V	4.826	3904.8 ±0.8	0.195	3.55	0.72	0.42
M2V	4.826	3688.6 ±1.4	0.153	2.17	0.59	0.57

Notes.

^(a)

g is the gravitational acceleration at the stellar surface in cgs units;

^(b)

temporal and spatial mean of the bolometric intensity normalised to the solar value;

^(c)

bolometric intensity contrast (temporal mean);

^(d)

z₀: = ⟨z(τ_R = 1) ⟩;

^(e)

z₂ is defined as the depth where ⟨p(z₂) ⟩ = 100 ⟨p(z₀) ⟩.

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