Preset Scenarios
0% (Peak Eclipse)
-100% (Ingress / Approach)
0% (Center Line)
+100% (Egress / Depart)
Perigee
Apogee
-1.5° South
+1.5° North
1. Orbital Geometry Cross-Section
Scale schematic: ray-traced Umbra, Penumbra & Antumbra projection
Sun Source
Moon (Occulting)
Earth Target
Penumbra / Umbral Cone
2. Earth Observer Sky View
Real-time telescope field view: Corona, Baily's Beads & Diamond Ring
Field of View: 1.2° Solar Disk
Corona Fully Visible
Solar Coverage (Obscuration)
100.0%
Shadow Cone Type
Umbra (Totality)
Apparent Angular Ratio
1.034 ×
Ambient Illuminance
0.15 Lux (Twilight)
How Celestial Alignment Dictates the Eclipse Experience
A solar eclipse occurs when the Moon transits directly between the Sun and Earth. Because the Moon’s orbit is elliptical (varying between perigee at ~356,400 km and apogee at ~406,700 km), its apparent angular size shifts relative to the Sun. When the Moon is near perigee, its apparent diameter exceeds the Sun's, casting a dark Umbra onto Earth (a Total Eclipse). Near apogee, the Moon is too small to cover the solar disc, creating an Antumbra with an annular "Ring of Fire". The 5.14° orbital inclination prevents eclipses at every new moon except when celestial nodes align.