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There is a growing evidence that several globular clusters must containmultiple stellar generations, differing in helium content. This hypothesis hashelped to interpret peculiar unexplained features in their horizontal branches.In this framework we model the peaked distribution of the RR Lyr periods in M3,that has defied explanation until now. At the same time, we try to reproducethe colour distribution of M3 horizontal branch stars. We find that only a verysmall dispersion in mass loss along the red giant branch reproduces with goodaccuracy the observational data. The enhanced and variable helium content amongcluster stars is at the origin of the extension in colour of the horizontalbranch, while the sharply peaked mass loss is necessary to reproduce thesharply peaked period distribution of RR Lyr variables. The dispersion in massloss has to be <~ 0.003 Msun, to be compared with the usually assumed values of~0.02 Msun. This requirement represents a substantial change in theinterpretation of the physical mechanisms regulating the evolution of globularcluster stars.

Is mass loss along the red giant branch of globular clusters sharply peaked? The case of M3