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The study of compact multi-planet systems has grown from a niche curiosity to a central pillar of planetary science. Modern observations reveal ensembles of small to mid-sized worlds orbiting within close quarters, sometimes in resonant configurations that hint at a shared migratory history. Theoretical work translates these patterns into a narrative where nascent planets form within evolving protoplanetary disks that change their density, temperature, and turbulence with time. In such environments, gravitational interactions between embryos and their gaseous surroundings guide growth trajectories, determine orbital spacings, and set the stage for long-term dynamical stability. This article synthesizes current ideas about how rapid disk evolution shapes the birth and early wandering of planetary systems.

A central question concerns how planetary cores accrete mass quickly enough to become solid, sizable bodies before the disk dissipates. The answer lies in a confluence of factors: pebbly material streaming through the disk, pressure traps that trap solids, and local enhancements of solid-to-gas ratios that expedite core growth. As cores gain mass, their gravity begins to sculpt nearby gas, opening gaps and altering the local flow of material. Migration becomes an inevitable consequence of disk–planet coupling, especially for rapidly evolving disks where shifts in viscosity, magnetic fields, and temperature gradients continually reorganize planetary orbits. Understanding these processes helps explain the observed compact configurations.

In rapidly evolving disks, the timeline of planet formation compresses compared with more quiescent disks. Turbulence, magnetically driven winds, and evolving ionization levels modulate the rate at which solids coagulate and migrate. Early planetesimals experience aerodynamic drag and gravitational nudges that determine their fate—whether they settle into stable orbits, collide and coalesce, or are ejected. As embryos reach pebble accretion thresholds, they can rapidly gain mass, potentially forming multiple planets in a relatively narrow annulus. The resulting mass spectrum and spacing depend on local disk properties, including surface density profiles and the presence of pressure bumps that can trap or repel drifting material. This interplay sets the architectural blueprint for compact systems.

Migration within evolving disks is not a single, uniform process; it is a tapestry woven from competing forces. Type I migration, driven by torques from density waves, can rapidly alter the orbital radii of low-mass planets. Yet, regions of outward migration may arise where surface density gradients or entropy effects reverse torque directions. As the disk evolves, these regions shift, sweeping planets through resonant corridors and capturing them into mean motion resonances or releasing them into broader orbits. Disk winds and photoevaporation gradually thin the disk, changing migration rates and timescales. In such dynamic contexts, the final layout of a compact system reflects a history of migrations that occurred during the fleeting lifetimes of their birthplaces.

Observationally, many compact systems exhibit near-resonant period ratios, suggesting a shared migratory past. Convergent migration—where outer planets move inward faster than inner ones—can trap planets into stable resonances, locking in distinctive orbital period relationships. However, resonant captures are not guaranteed; turbulence and stochastic forcing from disk inhomogeneities can disrupt or prevent strong resonances, leaving behind near-resonant or non-resonant configurations. The balance between smooth migration and random perturbations shapes whether a system settles into a harmonic chain or a more scattered arrangement. These outcomes depend sensitively on the disk’s lifetime, temperature structure, and the evolving mass distribution among the forming planets.

A complementary pathway involves rapid, differential growth among planetary embryos. When inner planets gain mass earlier from locally enhanced solid densities, they can carve out space for outer companions by modifying the gravitational potential in the disk or altering gas flow patterns. The resulting interaction network fosters intricate dynamical evolution, with orbit crossing, resonant repulsion, and damping through gas drag contributing to the final architecture. Numerical simulations show a spectrum of possible outcomes, from tightly knit chains to more loosely packed ensembles, each carrying a fossil record of the disk’s inward drift velocity, viscosity, and magnetic activity. The diversity observed in exoplanetary systems may thus reflect multiple, concurrent formation channels.

Beyond the immediate disk physics, the longer-term dynamical history matters as well. After disk dispersal, planets retain the memory of their birth environment in eccentricities, inclinations, and mutual inclinations. Residual planet–planet interactions can reshape orbits over millions of years, sometimes triggering late-stage instabilities that rearrange the system’s layout. The persistence of compact configurations implies that the primordial damping from the gas phase left behind a stable core, while still allowing some residual oscillations. Observational surveys of mature systems provide constraints on typical spacings, resonance occupancy, and mass distributions, which, in turn, feed back into models of disk evolution and migration. The synthesis across time scales is essential to explain why compact, multi-planet arrangements are so common.

A robust framework for formation models integrates three pillars: solid growth, gas-driven migration, and dynamical stabilization. Solid growth pathways, including pebble accretion and core–gas envelope capture, determine when planets reach masses capable of shaping their surroundings. Migration paths, molded by evolving disk properties, place planets into or near resonant configurations that may endure through disk dispersal. Finally, long-term dynamics influence whether a system remains stable or experiences rearrangements after the gas has vanished. This triad is tested by comparing synthetic planetary ensembles with observed exoplanet demographics, and it remains central to refining our understanding of how rapid disk evolution seeds compact architectures.

The observational side of the puzzle benefits from high-precision transit and radial velocity data, which reveal subtle signals of multiple planets in tight orbits. Statistical methods help distinguish genuine multi-planet signals from stellar activity, while transit timing variations illuminate gravitational interactions that betray resonances and mass ratios. Cross-matching planetary radii with stellar ages and metallicities informs theories about how disk chemistry influences planet formation efficiency. In rapidly evolving disks, one might expect stronger correlations between stellar properties and system compactness if disk lifetimes were the critical gating factor for formation. Emerging datasets continue to refine the empirical relationships that underpin theoretical scenarios.

Theoretical advances increasingly leverage population synthesis and machine-assisted exploration to map the wide range of plausible histories. By sampling varied disk lifetimes, accretion rates, and migration strengths, researchers generate ensembles that reproduce features of real systems, such as average spacings and resonance tendencies. These tools reveal which disk conditions most consistently yield compact, multi-planet arrangements and which populational outliers challenge conventional wisdom. Importantly, they also highlight degeneracies—distinct histories that produce similar end states—reminding us that present-day configurations encode a spectrum of possible birth environments. The ongoing synthesis is driving a more nuanced narrative of planetary assembly.

The field’s trajectory points toward an integrated picture in which rapid disk evolution acts as a primary sculptor of compact planetary systems. By combining robust disk physics with precise orbital dynamics, scientists aim to predict not only where planets reside but how their histories imprint observable traits such as transit timing residuals and resonant offsets. Interpreting these signals requires careful disentangling of competing processes—planet–disk coupling, planet–planet scattering, and external perturbations from nearby stars or nascent companions. As telescopes push toward fainter, younger systems and simulations gain realism, the gap between theory and observation narrows, enabling more confident inferences about the formation pathways that forge compact architectures.

In sum, compact multi-planet systems emerge from a dynamic interplay of evolving protoplanetary disks and migratory histories. The rapid changes in disk structure steer where solids concentrate, how quickly planets grow, and the manner in which their orbits migrate and interact. A wide spectrum of outcomes is possible, yet certain patterns—close spacing, resonant tendencies, and resilient stability—recur across observations and models. The pursuit of a unified explanation continues to advance with better data, more sophisticated simulations, and deeper theoretical insight into how migration histories etch the architecture of planetary systems that endure long after the gas has vanished.