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Rotation can substantially affect the life of stars \citep{Maeder:2009,Langer:2012}. From birth to death, the stellar plasma is expected to contain a substantial amount of angular momentum. During the long timescales of stellar evolution the internal distribution of angular momentum is expected to change and impact different observable properties of the star. Rotational instabilities and circulations can mix the star, changing its surface abundances \citep[see e.g.,][]{Meynet:2000,Maeder:2012}.   Redistribution of angular momentum occurs in the star due to structural changes. For example at the end of the main sequence most stars, after contracting due to the exhaustion of Hydrogen in their cores, ignite Hydrogen in a shell. Above this shell the star begin to expand, while the core continues its contraction.  in the structuThe total angular momentum is not conserved during the evolution, as stars are known to lose large amounts of mass (and angular momentum) through their stellar winds.  Depending on the coupling between the outer stellar layers and the stellar interiors, angular momentum loss (or distr  The final rotational properties of compact remnants   coor the interThe mixing surface rotation and composition, asteroseismic signat   .     lost through   mixing, s     changes during the long timescales of stellar evolution     is likely to change and affected by   in the stellar plasma plays a role in   setting different observable properties.   an impact on the   setting   non-negl rotation can affect the of a star.   structure and surface composition   It's massloss and activity massloss and surface composition of the star.   Rotation can have important effect The evolution of stars   mixing induced by some of the instabilities believed to be responsible for the bulk of angular momentum redistribution   by % coor the interThe mixing surface rotation and composition, asteroseismic signat   %by  rotation and magnetic fields generated in radiative zones (Spruit-Tayler dynamo) An %An  important test of our understanding of stellar physics calculation of the rotational evolution Therefore %Therefore  an important test of While %While  their pre-main sequence evolution is complex, a common assumption is that these stars reach a state of quasi-solid rotation when they start burning hydrogen at the zero age %age  main sequence. From there on the evolution has to account for the loss and the internal redistribution of angular momentum through d. Therefore stellar evolution models need to %to  include the important physical processes that dominate the angular momentum transport in the stellar interiors. Here we discuss how state-of-the-art stellar evolution calculations %calculations  of low-mass stars perform compared to some observational tests of their rotational properties. %Low-mass stars evolve past the main sequence toward their red giant stage. In this phase the star experience