Peak eclipse occurs at 13:25:23 UTC.

Use the timeline and city visibility tables on this page to compare UTC and local eclipse times for your timezone and major cities.

Solar eclipse visibility depends on the eclipse path and your location relative to total, annular, or partial zones.

The overall eclipse duration is about 2h 48m, including around 0 min of totality.

These are the four "contacts" — the precise moments when the Moon's and Sun's disks touch or separate: • C1 (First Contact): The Moon's edge first touches the Sun's edge. Partial eclipse begins — a small notch appears on the Sun's disk. • C2 (Second Contact): The Moon is now fully in front of the Sun. Totality (or annularity) begins. For a total eclipse this is the moment darkness falls and the corona becomes visible; for an annular eclipse, the "ring of fire" appears. • C3 (Third Contact): The Moon's edge reappears on the opposite side. Totality/annularity ends and partial eclipse resumes. • C4 (Fourth Contact): The Moon's edge leaves the Sun's disk entirely. The eclipse is over. Partial solar eclipses only have C1 and C4 — there is no totality, so C2 and C3 do not occur. The "C" simply stands for Contact.

Cloud cover, local horizon obstructions, and Moon altitude can all affect what you see. Higher Moon altitude generally improves viewing conditions for lunar eclipses.

Astronomers use strict definitions: "total" means the Moon completely covers the Sun (100.0%), and "partial" means anything less — even 99.9%. A city at 99.9% will see a dramatic darkening and most of the Sun hidden, but a thin sliver of sunlight remains visible around the Moon's edge. Only cities inside the narrow "path of totality" experience the full blackout, corona, and stars-in-daytime effect that makes a total eclipse extraordinary.

In a solar eclipse, the Moon passes between the Sun and Earth, casting a small, fast-moving shadow on Earth's surface. Only people inside that narrow shadow see the eclipse, which is why solar eclipses have a "path of totality." In a lunar eclipse, Earth passes between the Sun and the Moon, casting Earth's much larger shadow onto the Moon. Because the Moon is visible to everyone on the nightside of Earth at once, there's no moving shadow across the ground — everyone in the right hemisphere sees the same eclipse at the same time.

During a solar eclipse, the Moon's shadow is relatively small and sweeps across Earth's surface at over 1,000 mph. The dark line on the map traces this shadow's path. Cities directly on this path experience the full eclipse, while those farther away see only a partial eclipse.

The penumbra is the outer, lighter part of a shadow where the light source is only partially blocked. During a penumbral lunar eclipse, the Moon passes through Earth's penumbra — the Sun is partially obscured by Earth, causing a subtle dimming of the Moon rather than the dramatic red coloring seen in a total lunar eclipse. Penumbral eclipses are often difficult to notice with the naked eye. The word comes from the Latin "paene" (almost) and "umbra" (shadow) — literally "almost shadow."

The umbra is the darkest, central part of a shadow where the light source is completely blocked. During a total lunar eclipse, the Moon passes fully into Earth's umbra, causing the dramatic blood-red coloring as the only light reaching the Moon is bent and filtered through Earth's atmosphere. During a solar eclipse, the Moon's umbra is the small, dark core of its shadow — the narrow path on Earth where the Sun is completely covered. The word comes from the Latin for "shadow."

Totality is the phase of an eclipse where the covering body completely blocks the light source. In a total solar eclipse, totality is the awe-inspiring window — typically 1–7 minutes — when the Moon fully covers the Sun, revealing the solar corona, making stars visible in daytime, and causing a 360° sunset along the horizon. In a total lunar eclipse, totality is when the Moon is fully inside Earth's umbra and turns red or orange. Only locations directly within the path of totality (solar) or on the nightside of Earth (lunar) experience this phase.

An annular solar eclipse occurs when the Moon is near its farthest point from Earth (apogee) and appears slightly smaller in the sky than the Sun. At maximum eclipse, the Moon covers the center of the Sun but leaves a bright ring — called the "ring of fire" — visible around the Moon's edge. Unlike a total eclipse, an annular eclipse never reaches full darkness because the Sun is never completely covered. The word comes from the Latin "annulus" meaning ring.

Eclipse magnitude measures how much of the eclipsed body's diameter is covered at maximum eclipse. A magnitude of 1.0 means the covering body exactly matches the eclipsed body's apparent size. For solar eclipses, a magnitude greater than 1.0 produces totality; less than 1.0 produces a partial or annular eclipse. For lunar eclipses, magnitude measures how deeply the Moon enters Earth's shadow — above 1.0 means the Moon is fully inside the umbra (total eclipse). Magnitude is a dimensionless ratio of diameters, not area, so it's different from obscuration.

Obscuration is the fraction of the Sun's (or Moon's) area that is covered at any given moment, expressed as a percentage. Unlike magnitude (which measures diameter), obscuration measures the actual covered area. At 50% obscuration, half of the Sun's disk is blocked by the Moon. At 100%, the Sun is completely covered — but this only happens during totality in a total solar eclipse. In the City Visibility table, obscuration shows the maximum coverage that location will experience.