Context :

Aims : We investigate the impact of tidal interactions , before any mass transfer , on various properties of the stellar models .
We study the conditions for obtaining homogeneous evolution triggered by tidal interactions , and for avoiding any Roche lobe overflow during the Main-Sequence phase .
By homogeneous evolution , we mean stars evolving with a nearly uniform chemical composition from the center to the surface .

Methods : We consider the case of rotating stars computed with a strong coupling mediated by an interior magnetic field .
Models with initial masses between 15 and 60 M _ { \odot } , for metallicities between 0.002 and 0.014 , with initial rotation equal to 30 % and 66 % the critical rotation on the ZAMS are computed for single stars and for stars in close binary systems .
Close binary systems with initial orbital periods equal to 1.4 , 1.6 and 1.8 days and a mass ratio equal to 3/2 are considered .

Results : In models without any tidal interaction ( single stars and wide binaries ) , homogeneous evolution in solid body rotating models is obtained when two conditions are realized : the initial rotation must be high enough , the loss of angular momentum by stellar winds should be modest .
This last point favors metal-poor fast rotating stars .
In models with tidal interactions , homogeneous evolution is obtained when rotation imposed by synchronization is high enough ( typically a time-averaged surface velocities during the Main-Sequence phase above 250 km s ^ { -1 } ) , whatever the mass losses .
We give plots indicating for which masses of the primary and for which initial periods , the conditions for the homogenous evolution and for the avoidance of the Roche lobe overflow are met , this for different initial metallicities and rotations .
In close binaries , mixing is stronger at higher than at lower metallicities .
Homogeneous evolution is thus favored at higher metallicities .
Roche lobe overflow avoidance is favored at lower metallicities due to the fact that stars with less metals remain more compact .
We study also the impact of different processes for the angular momentum transport on the surface abundances and velocities in single and close binaries .
In models where strong internal coupling is assumed , strong surface enrichments are always associated to high surface velocities in binary or single star models .
In contrast , models computed with mild coupling may produce strong surface enrichments associated to low surface velocities .
This observable difference can be used to probe different models for the transport of the angular momentum in stars .
Homogeneous evolution is more easily obtained in models ( with or without tidal interactions ) with solid body rotation .

Conclusions : Close binary models may be of interest for explaining homogeneous massive stars , fast rotating Wolf-Rayet stars , and progenitors of long soft gamma ray bursts , even at high metallicities .