Dynamical evolution and dissolution timescale of young stellar clusters in the Orion star-forming complex

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ID: 317077
2026
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Abstract
Abstract We present a comprehensive analysis of the Orion star-forming complex (OSFC), combining structural, kinematic, and dynamical information to constrain the present-day state and future evolution of its stellar substructures. Using Gaia DR3 astrometry and complementary radial velocities from high-resolution spectroscopic surveys, we derived three-dimensional velocity distributions and structural parameters for 13 young clusters. For the stellar component, we estimated a correction of the present-day mass function for observational incompleteness and calculated the virial state, αvir, finding that all clusters are supervirial. Direct N-body simulations initialized from the present-day global parameters and evolved for 300 Myr in a Galactic potential suggest a separation of the OSFC clusters into two regimes: seven clusters with αvir ≲ 7 evolve in a Galactic-potential-regulated regime that retains a bound core for ≳ 170 Myr as long-lived open clusters, whereas six clusters with αvir ≳ 7 enter an internal-dynamics–dominated regime, dissolving before 120 Myr and rapidly populating the Galactic stellar field. For both regimes, a control test indicates negligible cluster–cluster interactions under current OSFC conditions. Finally, long-lived clusters show low-amplitude modulations in the bound fraction correlated with the Galactic vertical motion, consistent with disk-crossing tidal heating and the temporary recapture of marginal members. These results highlight the OSFC as a natural laboratory where heterogeneous initial conditions give rise to persistent open clusters and dispersing groups.
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Authors Sergio Sánchez-Sanjuán, Ángeles Pérez-Villegas, Jesús Hernández, Luis Aguilar
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1098
URL
https://doi.org/10.1093/mnras/stag1098
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