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Recent studies of low- and intermediate-mass stars show that the evolution ofthe chemical elements in these stars is very different from that proposed bystandard stellar models. Rotation-induced mixing modifies the internal chemicalstructure of main sequence stars, although its signatures are revealed onlylater in the evolution when the first dredge-up occurs. Thermohaline mixing islikely the dominating process that governs the photospheric composition oflow-mass red giant branch stars and has been shown to drastically reduce thenet 3He production in these stars. The predictions of these new stellar modelsneed to be tested against galaxy evolution. In particular, the resultingevolution of the light elements D, 3He and 4He should be compared with theirprimordial values inferred from the Wilkinson Microwave Anisotropy Probe dataand with the abundances derived from observations of different Galacticregions. We study the effects of thermohaline mixing and rotation-inducedmixing on the evolution of the light elements in the Milky Way. We computeGalactic evolutionary models including new yields from stellar models computedwith thermohaline instability and rotation-induced mixing. We discuss theeffects of these important physical processes acting in stars on the evolutionof the light elements D, 3He, and 4He in the Galaxy. Galactic chemicalevolution models computed with stellar yields including thermohaline mixing androtation fit better observations of 3He and 4He in the Galaxy than modelscomputed with standard stellar yields. The inclusion of thermohaline mixing instellar models provides a solution to the long-standing "3He problem" on aGalactic scale. Stellar models including rotation-induced mixing andthermohaline instability reproduce also the observations of D and 4He.

Effects of thermohaline instability and rotation-induced mixing on the evolution of light elements in the Galaxy : D, 3He and 4He