Pebble accretion efficiency vs planet eccentricity. The default run is shown in black, with M_p = 0.1 M_⊕, M_⋆ = 1 M_⊙, v_hw = 30 m s⁻¹ and τ_s = 10⁻². In each panel one parameter varies and the other three keep the same. Upper left panel: three different planet masses, M_p = 1 M_⊕, M_p = 0.1 M_⊕ and M_p = 0.01 M_⊕; upper right panel: three different stellar masses, M_⋆ = 3 M_⊙, M_⋆ = 1 M_⊙ and M_⋆ = 0.3 M_⊙; lower left panel: three different headwind velocities, v_hw = 15 m s⁻¹, v_hw = 30 m s⁻¹ and v_hw = 60 m s⁻¹; lower right panel: three dimensionless stopping times, τ_s = 10⁻³, τ_s = 10⁻² and τ_s = 10⁻¹. The dot gives the mean value, and the errorbar indicates the Poisson counting error. The solid line is the analytical fit of Eq. (16). The efficiency increases with M_p, and decreases with M_⋆, v_hw and τ_s.