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By examining the diffusion of young white dwarfs through the core of theglobular cluster 47 Tucanae, we estimate the time when the progenitor star lostthe bulk of its mass to become a white dwarf. According to stellar evolutionmodels of the white-dwarf progenitors in 47 Tucanae, we find this epoch tocoincide approximately with the star ascending the asymptotic giant branch($3.0 \pm 8.1$ Myr before the tip of the AGB) and more than ninety millionyears after the helium flash (with ninety-percent confidence). From thediffusion of the young white dwarfs we can exclude the hypothesis that the bulkof the mass loss occurs on the red-giant branch at the four-sigma level.Furthermore, we find that the radial distribution of horizontal branch stars isconsistent with that of the red-giant stars and upper-main-sequence stars andinconsistent with the loss of more than 0.2 solar masses on the red-giantbranch at the six-sigma level.

When do stars in 47 Tucanae lose their mass?