The Dynamical Evolution of the Pleiades
Joseph M. Converse, Steven W. Stahler

TL;DR
This study uses numerical simulations to trace the Pleiades' dynamical evolution from just after gas expulsion to future dissolution, revealing how binary interactions and galactic tides shape its structure over time.
Contribution
It provides a detailed dynamical model of the Pleiades' evolution, including initial conditions, binary effects, and future tidal disruption, extending previous static analyses.
Findings
Original cluster had a virial radius of 4 pc.
Binary interactions significantly influenced cluster expansion.
Future evolution involves continued expansion and tidal stripping.
Abstract
We present the results of a numerical simulation of the history and future development of the Pleiades. This study builds on our previous one that established statistically the present-day structure of this system. Our simulation begins just after molecular cloud gas has been expelled by the embedded stars. We then follow, using an N body code, the stellar dynamical evolution of the cluster to the present and beyond. Our initial state is that which evolves, over the 125 Myr age of the cluster, to a configuration most closely matching the current one. We find that the original cluster, newly stripped of gas, already had a virial radius of 4 pc. This configuration was larger than most observed, embedded clusters. Over time, the cluster expanded further and the central surface density fell by about a factor of two. We attribute both effects to the liberation of energy from tightening…
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