Copyright by Athena Ranice Stacy 2011 - The University of Texas at ...

growth of Lacc can be seen in Fig. 2.12. The discontinuous slope in the ac-
cretion luminosity is an artefact of our approximate modelling of protostellar
structure.
Since the accretion luminosity does not exceed either Eddington lumi-
nosity, we conclude that for the duration of our simulation, radiation pressure
is not likely to significantly change the early accretion rates we have found. At
later times, when the protostar reaches higher masses, however, and in partic-
ular when it reaches the ZAMS and hydrogen burning turns on, such feedback
effects will become more important, and can no longer be neglected.
2.5 Parameter Sensitivity
How commonly do Pop III stars form in multiples? To what extent does
this result depend on the initial cosmological parameter values, particularly
the value for σ8? Is there a relation between the spin of a minihalo and the
probability that it will host a Pop III multiple (see section 4.1)? To address
this uncertainty, we make an initial estimate of the sensitivity of our results
to differing values of σ8 by comparing the specific angular momentum profile
of the central 1000 M⊙ of our simulation with that of Abel et al. (2002) and
Yoshida et al. (2006) (Fig. 2.13). The angular momentum profile for our work
is taken at the point immediately before the first sink forms. Abel et al. (2002)
initialized their simulation using h=0.5, ΩΛ = 0, ΩB = 0.06 and σ8 = 0.7.
Yoshida et al. (2006) used h=0.7, ΩΛ = 0.7, ΩB = 0.04 and σ8 = 0.9. If
the particular parameter values used in initializing our calculation made the
central gas more prone to develop a flattened disk-like structure that would
later fragment, this would first be apparent in an enhanced angular momentum
profile. However, despite the varying initial conditions used for each of these
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