During totality, the Moon will not disappear. Instead, it will shift into copper and deep red wavelengths. This coloration results from Rayleigh scattering in Earth’s atmosphere, which preferentially scatters shorter blue wavelengths while allowing longer red wavelengths to refract into the umbra and illuminate the Moon. The exact hue depends on global atmospheric conditions, including aerosol concentration from dust or volcanic activity. Key technical phases: • Penumbral eclipse: The Moon enters Earth’s penumbra; subtle dimming begins. • Partial eclipse: The Moon begins entering the umbra; a curved shadow becomes visible. • Totality: The Moon is fully immersed in the umbra; red coloration peaks. • Egress: The sequence reverses as the Moon exits the umbra and penumbra. Because lunar eclipses are visible from anywhere on Earth where the Moon is above the horizon, their audience footprint is far larger than that of solar eclipses. No specialized equipment is required, though binoculars...