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\bf{Abstract} {\bf Abstract}  Stars are born rotating. Observations of stars on their main sequence reveal that the majority of stars with mass above $\sim 1.5\mso$ are spinning fairly rapidly. 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 main sequence. From there on their evolution has to account for the loss and the internal redistribution of angular momentum. Therefore stellar evolution models need 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 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