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SUMMARY:Quantifying the Effect of a Bottom-Light IMF on Globular Cluster E
 volution Using the Cluster Monte Carlo Code
DTSTART;VALUE=DATE-TIME:20261028T181700Z
DTEND;VALUE=DATE-TIME:20261028T181800Z
DTSTAMP;VALUE=DATE-TIME:20261024T120149Z
UID:indico-contribution-3682@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Kristen Cowan (Saint Mary's University)\nThe distrib
 ution of stellar masses within a globular cluster (GC) at the time of form
 ation\, referred to as the Initial Mass Function (IMF)\, is directly linke
 d to the evolution of the cluster\, including the rate of binary black hol
 e (BH) mergers that produce gravitational waves. Recent studies suggest th
 at GCs may have formed with a bottom-light IMF\, meaning fewer low mass st
 ars and more BH progenitors per unit cluster mass compared to the standard
  Kroupa (2001) IMF. In this study\, we evolve a small set of simulated GCs
  with a bottom-light IMF using the Cluster Monte Carlo code\, which models
  the dynamical interactions between stars\, the formation and retention of
  compact objects and the large-scale evolution of the cluster mass and rad
 ius. We then compare the evolutionary data to an identical set of clusters
  formed with the standard Kroupa IMF to quantify the effect of the varying
  mass distribution. By analysing properties including black hole populatio
 ns\, cluster mass and radius over time\, we investigate whether a bottom-l
 ight IMF produces properties of evolved GCs that differ significantly from
  those produced by a Kroupa IMF. The results of these simulations can be c
 ompared to current photometric observations to inform future work surround
 ing the IMF and help revise predictions for the rates of binary BH mergers
  originating in GCs.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributi
 ons/3682/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3682/
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