Jc. Lombardi et al., COLLISIONS OF MAIN-SEQUENCE STARS AND THE FORMATION OF BLUE STRAGGLERS IN GLOBULAR-CLUSTERS, The Astrophysical journal, 468(2), 1996, pp. 797-818
We report the results of new SPH calculations of parabolic collisions
between two main-sequence stars in a globular cluster. Such collisions
are directly relevant to the formation of blue stragglers. In particu
lar, we consider parent stars of mass M/M(TO)=0.2, 0.5, 0.75, and 1, w
here M(TO) is the cluster turnoff mass (typically about 0.8 M.). The p
arent star models are more realistic, and the numerical resolution of
the hydrodynamics more detailed, than in previous studies. We focus on
the hydrodynamic mixing of helium and hydrogen, which plays a crucial
role in establishing the color, luminosity, and lifetime of collision
al blue stragglers. In all cases we find negligible hydrodynamic mixin
g of helium into the outer envelope of the merger remnant. The amount
of hydrogen carried into the core of the merger remnant depends strong
ly on the entropy profiles of the colliding stars. For stars with near
ly equal masses (and hence entropy profiles), the composition profile
of the remnant closely resembles that of the parents. If the parent st
ars were close to turnoff, very little hydrogen is present at the cent
er of the merger remnant and the main-sequence lifetime of the blue st
raggler could be short. In contrast, during a collision between stars
with sufficiently different masses (mass ratio q less than or similar
to 0.5), the hydrogen-rich material originally in the smaller star mai
ntains, on average, a lower specific entropy than that of the more mas
sive star and therefore settles preferentially in the core of the merg
er remnant. Through this process, moderately massive blue stragglers (
with masses M(TO)less than or similar to M(BS)less than or similar to
1.5M(TO)) can obtain a significant supply of fresh hydrogen fuel, ther
eby extending their main-sequence lifetime. We conclude, in contrast t
o what has often been assumed, that blue stragglers formed by direct s
tellar collisions do not necessarily have initially homogeneous compos
ition profiles. However, we also demonstrate that the final merged con
figurations, although close to hydrostatic equilibrium, are typically
far from thermal equilibrium. Therefore, it is possible that convectiv
e, semiconvective, or rotationally induced mixing could occur on a the
rmal timescale, as the merger remnant recontracts to the main sequence
.