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We explore the evolution of collisionally merged stars in the blue stragglerregion of the HR diagram. The starting models for our stellar evolutioncalculations are the results of the smoothed particle hydrodynamics (SPH)simulations of parabolic collisions between main sequence stars performed byLombardi, Rasio and Shapiro (1996). Since SPH and stellar evolution codesemploy different and often contradictory approximations, it is necessary totreat the evolution of these products carefully. The mixture and disparity ofthe relevant timescales (hydrodynamic, thermal relaxation and nuclear burning)and of the important physical assumptions between the codes makes the combinedanalysis of the problem challenging, especially during the initial thermalrelaxation of the star. In particular, the treatment of convection isimportant, and semiconvection must be modeled in some detail.  The products of seven head-on collisions are evolved through their initialthermal relaxation, and then through the main sequence phase to the base of thegiant branch. Their evolutionary tracks are presented. In contrast to theassumptions in previous work, these collision products do not developsubstantial convective regions during their thermal relaxation, and thereforeare not mixed significantly after the collision.Comment: 45 pages, 8 figures (encapsulated postscript), uses AASTeX, to be  published in Astrophysical Journal volume 48

Evolution of Stellar Collision Products in Globular Clusters. I. Head‐on Collisions