Disk fraction as a function of period (black circles) for BDs (left panels) and VLM stars (right panels) at 2.1 Myr (top panels) and at 3.1 Myr (bottom panels). The period bins are P ≤ 2.5 d, 2.5 d < P ≤ 5.0 d, and P > 5.0 d for BDs and P ≤ 2.5 d, 2.5 d < P ≤ 5.0 d, 5.0 d < P ≤ 7.5 d, and P > 7.5 d for VLM stars. Our simulations at 2.1 Myr are compared to observations of the ONC by RL10 (red squares) and D14 (blue triangles) and, at 3.1 Myr, they are compared to the combined σ Ori sample of S04 and C10 (red squares) The model’s error bars are equal to 1σ above and below the fraction value and they were calculated through resampling. The RL10 error bars were obtained from Rodríguez-Ledesma et al. (2010). For the observational sample at 3.1 Myr, the error bars were calculated following the Bayesian approach of Burgasser et al. (2003).