Coupled Disk and Dynamical Processes Shaping Exoplanetary Systems

Exoplanet surveys reveal a remarkable diversity in planetary system architectures, ranging from

compact super-Earth multiples to widely spaced, eccentric giant planets. This paper presents an

integrated framework linking initial protoplanetary disk conditions, planet formation mechanisms,

disk-driven migration, and post-disk dynamical evolution to observed orbital configurations.

Variations in disk structure, thermodynamics, and angular momentum transport set the initial

planetary architecture, while gravitational interactions, resonant coupling, and dynamical

instabilities after gas dispersal amplify small differences, producing divergent long-term outcomes.

Observed trends in eccentricity, orbital spacing, multiplicity, and resonance occupancy reflect the

combined imprint of initial disk conditions and subsequent N-body evolution. We examine

observational constraints from transit, radial velocity, and high-resolution millimeter surveys,

highlighting selection biases and their implications for theoretical modeling. Our results

demonstrate that architectural diversity is an intrinsic outcome of coupled disk and dynamical

processes, rather than the result of rare or external perturbations. This framework offers a

physically grounded approach for interpreting exoplanet demographics and understanding the

dominant processes shaping planetary system evolution.