Computed Physical Properties, Orbital Architecture, and Dynamical Assessment of the TOI-5624 Multiplanetary System
Abstract
The characterization of compact multiplanetary systems provides important insights into planetary structure, orbital architecture, irradiation environments, and long-term dynamical stability. In this work, the newly confirmed TOI-5624 system is investigated as a five-planet system composed of TOI-5624 b, c, d, e, and f. The analysis is based on observational data from the NASA Exoplanet Archive, combined with a reproducible Python-based computational framework. A set of physical, orbital, thermal, and first-order dynamical parameters is examined, including semi-major axis, orbital period, planetary mass and radius, bulk density, equilibrium temperature, stellar flux, surface gravity, escape velocity, period ratios between successive planets, and mutual Hill separations. Semi-major axes are independently calculated using Kepler’s third law and compared with archive values, showing excellent agreement with differences below approximately 0.11 percent. The results indicate that TOI-5624 is a compact multiplanetary system with planets distributed between approximately 0.042 AU and 0.237 AU. The orbital period ratios between successive planets are approximately 2.326, 1.741, 1.565, and 2.111, suggesting a non-resonant but dynamically ordered architecture with near-commensurabilities. The mutual Hill separation analysis shows that all adjacent planet pairs exceed both the classical two-planet Hill-stability limit of 2√3 and the conservative empirical spacing threshold of Δ=10, indicating that the nominal system architecture is well separated against immediate close encounters at the first-order level. The equilibrium temperatures range from about 478.5 K to 1136 K, while the incident stellar flux spans from approximately 8.7 to more than 275 times the Earth’s flux, indicating a strongly irradiated system with no planet in an Earth-like habitable environment. This study provides a consistent computational characterization of the TOI-5624 system and demonstrates a reproducible first-order framework for examining the physical properties, irradiation environment, orbital architecture, and dynamical spacing of newly confirmed compact multiplanetary systems.