The Search for Vulcanoids: A Comprehensive Analysis

Our understanding of the architecture of the Solar System has grown significantly in recent decades. The discovery and characterisation of various asteroid populations have provided fundamental insights into the nature and origins of minor bodies. However, among the few stable dynamical niches that remain largely unexplored today is the region interior to Mercury’s orbit, where the Vulcanoid Asteroids are hypothesised to reside. This Master's Thesis presents a comprehensive analysis of the Vulcanoid Zone, combining theoretical dynamical models with future observational strategies. The orbital boundaries and the extreme thermal and collisional environment of this intra-Mercurial region are investigated, highlighting how continuous collisional grinding and non-gravitational forces heavily constrain the survival of primordial material. Despite these critical conditions, the existence of kilometer-scale fragments cannot be definitively ruled out on theoretical grounds alone. To address the historical challenges of observing objects in such close proximity to the Sun, this thesis conducts a detailed signal-to-noise ratio (SNR) analysis and, based on these constraints, a specific observational mission profile tailored for the upcoming total solar eclipse on August 2, 2027, is proposed. By outlining the required optical systems and detection strategies, this work provides a concrete pathway for either discovering these elusive objects or placing rigorous limits on their population, thereby advancing our understanding of the early formation of the inner Solar System. Original contributions include the development of an eclipse-specific signal-to-noise model, the construction of a Vulcanoid detectability map combining all major observational limits, and the design of dedicated observing campaigns for the 2026 and 2027 total solar eclipses.