An evolutionary sequence is presented for a star of 1 19 M , with composition parameters (X, Z) = ( , ). The evolution was followed from the main sequence to the onset of convection in the core during the helium flash. The resulting core mass at the helium flash, Me = M is smaller than those found for Population II stars with the same helium abundance. No mixing between hydrogen-rich envelope and the helium core can be expected due to the non-central development of the flash. The clumping of stars on the giant branch of old open clusters, discussed by Cannon, is considered.