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Article overview
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On the true shape of the upper end of the stellar initial mass function: The case of R136 | Sambaran Banerjee
; Pavel Kroupa
; | Date: |
18 Sep 2012 | Abstract: | Context: The shape of the stellar initial mass function (IMF) of a star
cluster near its upper mass limit is a focal topic of investigation as it
determines the high mass stellar content and hence the dynamics of the cluster
at its embedded phase as well as during its young gas-free phase. The massive
stellar content of a young cluster, however, can be substantially modified due
to the dynamical ejections of the massive stars so that the present-day
high-mass stellar mass function (hereafter MF) can be different than that with
which the cluster is born. Aims: In the present study, we provide a preliminary
estimate of this evolution of the high-mass IMF of a young cluster due to early
ejections of massive stars, using the Large Magellanic Cloud massive, young
cluster R136 as an example. Methods: To that end, we utilize the results of the
state-of-the-art calculations by Banerjee, Kroupa & Oh (2012) comprising direct
N-body computations of realistic, binary-rich, mass-segregated models of R136.
In particular, these calculations provide the ejection fraction of stars as a
function of stellar mass. Results: We find that if the measured IMF of R136 is
granted to be canonical, as observations indicate, then the "true" high-mass
IMF of R136 at its birth must be at least moderately top-heavy when corrected
for the dynamical escape of massive stars. Conclusions: The top-heaviness of
the true high-mass IMF over the observationally determined one is a general
feature of massive, young clusters where the dynamical ejection of massive
stars is efficient. We discuss its implications and possible improvements over
our current estimate. | Source: | arXiv, 1209.4079 | Services: | Forum | Review | PDF | Favorites |
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