THE LUMINOSITY FUNCTIONS OF EMBEDDED STELLAR CLUSTERS .2. NUMERICAL RESULTS

We use the theory developed previously to calculate the evolving luminosity functions of very young stellar clusters. The luminosity function of the protostars alone quickly attains a characteristic, sharply peaked shape, which it maintains throughout the time of cluster formation. For the pre-main-sequence stars, the function continually changes but displays a pronounced ''step'' near a luminosity of 10 L. for a prolonged period. At most times, the vast majority of cluster members are pre-main-sequence stars. However, the total cluster luminosity is dominated first by the protostellar and later by the main-sequence component. At these late times, it is the brightest stars which reach the main sequence first. Finally, a preliminary application of our model to the rho Ophiuchi embedded cluster indicates that star formation has proceeded in that region for 1 x 10(6) yr.