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Fig. 11


Derived mass accretion rates as a function of the age of the PMS stars. Stars with masses higher and lower than 0.6 M are shown separately. The large black dots are for the stars in Tr 14, whereas the smaller grey dots correspond to objects in Tr 37. The solid line shows the temporal evolution of acc for viscous discs as predicted by Hartmann et al. (1998).

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