Optical modeling demonstrates lunar occultation achieves a 5.066 x 10^-13 B_sun stray-light rejection ratio in coronagraphy, suggesting unprecedented inner solar corona imaging capabilities.
The Lunar Far-Side Solar Observatory (LF-SCSN) architecture resolves a fundamental limit in space coronagraphy: instrument-induced diffraction glare that obscures the critical inner solar corona (1.05 R_sun to 2.5 R_sun). While state-of-the-art space missions rely on manufactured occulting discs capped at stray-light suppression floors of ~10^-6 to 10^-7 B_sun, LF-SCSN utilizes the 3,474.8 km physical sphere of the Moon as a natural external occulter. Placed in a Highly Eccentric Lunar Orbit (HELO) with an aposelene altitude of 15,636 km (10 R_M), the spacecraft operates inside the deep geometric umbral shadow cone. Classical wave-optics Fresnel diffraction yields a stray-light rejection ratio of 5.066 x 10^-13 B_sun—a 6.2 to 7.1 order-of-magnitude improvement over hardware occulters. This white paper establishes the mathematical proof, orbital mechanics model, Science Traceability Matrix (STM), payload specifications, and telemetry architecture for submission to space agency solicitations.
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Robert Andrew Woodgate (2026) studied this question.
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