On the Effects of Subvirial Initial Conditions and the Birth Temperature
  of R136
  We investigate the effect of different initial virial temperatures, Q, on the
dynamics of star clusters. We find that the virial temperature has a strong
effect on many aspects of the resulting system, including among others: the
fraction of bodies escaping from the system, the depth of the collapse of the
system, and the strength of the mass segregation. These differences deem the
practice of using "cold" initial conditions no longer a simple choice of
convenience. The choice of initial virial temperature must be carefully
considered as its impact on the remainder of the simulation can be profound. We
discuss the pitfalls and aim to describe the general behavior of the collapse
and the resultant system as a function of the virial temperature so that a well
reasoned choice of initial virial temperature can be made. We make a correction
to the previous theoretical estimate for the minimum radius, $R_{min}$, of the
cluster at the deepest moment of collapse to include a Q dependency,
$R_{min}\approx Q + N^{(-1/3)}$, where $N$ is the number of particles.
  We use our numerical results to infer more about the initial conditions of
the young cluster R136. Based on our analysis, we find that R136 was likely
formed with a rather cool, but not cold, initial virial temperature ($Q\approx
0.13$). Using the same analysis method, we examined 15 other young clusters and
found the most common initial virial temperature to be between 0.18 and 0.25.
