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(abridged) Numerous spectroscopic observations provide compelling evidencefor non-canonical processes that modify the surface abundances of low- andintermediate-mass stars beyond the predictions of standard stellar theory. Westudy the effects of thermohaline instability and rotation-induced mixing inthe 1-4 Msun range at solar metallicity. We present evolutionary models byconsidering both thermohaline and rotation-induced mixing in stellar interior.We discuss the effects of these processes on the chemical properties of starsfrom the zero age main sequence up to the end of the second dredge-up on theearly-AGB for intermediate-mass stars and up to the AGB tip for low-mass stars.Model predictions are compared to observational data forlithium,12C/13C,[N/C],[Na/Fe],16O/17O, and 16O/18O in Galactic open clustersand in field stars with well-defined evolutionary status,as well as inplanetary nebulae. Thermohaline mixing simultaneously accounts for the observedbehaviour of 12C/13C,[N/C], and lithium in low-mass stars that are moreluminous than the RGB bump, and its efficiency is increasing with decreasinginitial stellar mass. On the TP-AGB,thermohaline mixing leads to lithiumproduction, although the 7Li yields remain negative. Although the 3He stellaryields are much reduced thanks to this process, we find that solar-metallicity,low-mass stars remain net 3He producers. Rotation-induced mixing is found tochange the stellar structure so that in the mass range between \sim 1.5 and 2.2Msun the thermohaline instability occurs earlier on the red giant branch thanin non-rotating models. Finally rotation accounts for the observed star-to-starabundance variations at a given evolutionary status, and is necessary toexplain the features of CN-processed material in intermediate-mass stars.

Thermohaline instability and rotation-induced mixing. I - Low- and intermediate-mass solar metallicity stars up to the end of the AGB