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We present new binary stellar evolution models that include the effects oftidal forces, rotation, and magnetic torques with the goal of testing PlanetaryNebulae (PNe) shaping via binary interaction. We explore whether tidalinteraction with a companion can spin up the AGB envelope. To do so we haveselected binary systems with main sequence masses of 2.5 \Mo and of 0.8 \Mo andevolve them allowing initial separations of 5, 6, 7, and 8 AU. The binarystellar evolution models have been computed all the way to the PNe formationphase or until Roche lobe overflow (RLOF) is reached, whatever happens first.We show that with initial separations of 7 and 8 AU, the binary avoids enteringinto RLOF, and the AGB star reaches moderate rotational velocities at thesurface ($\sim 3.5 $ and $\sim 2 $ \kms respectively) during the inter-pulsephases, but after the thermal pulses it drops to a final rotational velocity ofonly $\sim 0.03 $ \kms. For the closest binary separations explored, 5 and 6AU, the AGB star reaches rotational velocities of $\sim 6 $ and $\sim 4 $ \kmsrespectively when the RLOF is initiated. We conclude that the detached binarymodels that avoid entering the RLOF phase during the AGB will not shape bipolarPNe, since the acquired angular momentum is lost via the wind during the lasttwo thermal pulses. This study rules out tidal spin-up in non-contact binariesas a sufficient condition to form bipolar PNe.

Rotating Stars and the Formation of Bipolar Planetary Nebulae II: Tidal Spin-up