Orbitallides

Orbitallides are a hypothetical class of celestial bodies that are thought to exist in orbits around stars other than our Sun. The term itself is a portmanteau of "orbit" and "satellite," suggesting a celestial object in orbit. While no direct observation of an orbitallide has ever been made, their existence is theorized as a possible explanation for certain anomalies in the gravitational fields of exoplanetary systems.

The concept of orbitallides primarily stems from the study of orbital resonances and the distribution of mass within planetary systems. If a significant amount of matter were to aggregate in a stable orbital path around a star, it could exert gravitational influence that might be detected by observing the subtle perturbations in the orbits of known planets. These hypothetical bodies could range in size from small, asteroid-like objects to larger, moon-sized entities.

Several theoretical models propose mechanisms by which such orbitallides might form. These include the gradual accretion of interstellar dust and gas in stable orbital zones, or perhaps the capture of rogue objects that stray into a star's gravitational well. Further research into the dynamics of exoplanetary systems and advancements in observational astronomy are necessary to either confirm or refute the existence of orbitallides.