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

We use the theory developed previously to calculate the evolving lumin osity functions of very young stellar clusters. The luminosity functio n of the protostars alone quickly attains a characteristic, sharply pe aked shape, which it maintains throughout the time of cluster formatio n. For the pre-main-sequence stars, the function continually changes b ut displays a pronounced ''step'' near a luminosity of 10 L. for a pro longed period. At most times, the vast majority of cluster members are pre-main-sequence stars. However, the total cluster luminosity is dom inated first by the protostellar and later by the main-sequence compon ent. At these late times, it is the brightest stars which reach the ma in sequence first. Finally, a preliminary application of our model to the rho Ophiuchi embedded cluster indicates that star formation has pr oceeded in that region for 1 x 10(6) yr.