Fig. 1
Time evolution of the stellar luminosity after Baraffe et al. (1998) and the evolution of Ṁ after Hartmann et al. (1998). The luminosity of the star reduces by a factor of 3 in 10 Myr and the accretion rate reduces by over 2 orders of magnitude during the same time period. However, an accretion rate of Ṁ = 1 × 10-9 M⊙/yr is already reached after 5 Myr when the disc can be cleared by photo evaporation.
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