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6 Color-magnitude diagram for the globular cluster M3, with a superposed schematic evolutionary path. L. R. Sandage, J056, and M. Schwar:zschild, Sc70. 6 _8 B- V it moves off the main sequence. In comparison to their size on the main sequence, the stars now become giants. Their radii can increase by factors of 10 or 100. Let us see how such stages evolve. For this purpose the study of globular clusters is most instructive. These clusters contain what are believed to be so me of the oldest stars in the Galaxy.

They contain a large fraction of their mass in the form of hydrogen and are able to retain it because of the low temperatures determined by their relatively large distances from the sun and because of their stronger gravitational fields. This distribution by volatility suggests that elements with low vapor pressures were able to solidify at small distances from the sun in the early life of a gaseous protoplanetary nebula surrounding the sun. Initially the size of condensations may have been no bigger than dust grains, but these grains could have aggregated by successive collisions, some of which would have vaporized both colliding grains, while others would have caused the grains to stick.

The chemical makeup of the outermost portions of the star, the only portions we actually see, therefore shows no evidence of the complicated changes that have occurred in the star's interior, even at this advanced stage of evolution. During this asymptotic giant branch stage EF, the star folIo ws almost the same path through the H-R diagram that it traced out before in going from C to D and in the top portion of the track from B to C. These three different groups have an outwardly similar appearance.

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