N -body simulations of the open cluster population in the Milky Way and the impact of GMC encounters

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ID: 327364
2026
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Abstract
Abstract We investigate the population of open clusters in the Solar Neighbourhood and model the effect of encounters with giant molecular clouds (GMCs) over the last 1 Gyr. We combine a Galactic model with N-body simulations of 20692 unique clusters in the mass range [50 − 24000] M⊙. Each cluster is simulated twice: with and without tidal forces from the GMCs. We find that an initial cluster mass function truncated at ~9000 M⊙ best reproduces the observed mass function evolution. For the age function, the observations show a decline in clusters for ages older than ~1 Myr, whereas our simulated clusters show a decline after ~50 Myr. The observed early disruption suggests that some clusters form supervirial, whereas our simulated clusters are created in virial equilibrium. Low-mass (<600 M⊙) clusters are most sensitive to GMC encounters, which accelerate their disruption in the first ~200 Myr. After ~500 Myr, the impact of GMCs becomes irrelevant since the clusters will have been destroyed regardless of whether they experience GMC encounters or not. The survival of intermediate-mass (600 − 6000 M⊙) clusters is significantly reduced by GMCs at ages up to 1 Gyr. High-mass (>6000 M⊙) clusters survive to 1 Gyr with minimal disruption with or without GMCs. We find that clusters that have had strong GMC encounters within the last 20 Myr should have tidal tails that are randomly orientated with respect to the Galactic centre.
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Authors Timmi G Jørgensen, Ross P. Church
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Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1641
URL
https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stag1641/70870438/stag1641.pdf
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