Stellar evolution in early phases of gravitational contraction.

The surface condition for red giant stars worked out in the previous paper indicates that stars lie in the low luminosity and low temperature region of the H-R diagram cannot be in equilibrium so that the evolutional path of contracting stars in this region will be different from that calculated by HENYEY et al. The age of these stars along the loci of quasi-static solutions is calculated. The result `seems to explain well the H-R diagram of a young cluster NGC 2264.