NASA-derived eclipse geometry

2027 solar eclipse path of totality

The August 2, 2027 path of totality crosses southern Spain and Gibraltar, continues across North Africa, then reaches the Arabian Peninsula. Near greatest eclipse, the path is about 258 km wide and central totality lasts a little over 6 minutes 23 seconds.

Eclipse Wayfinder uses NASA-derived centerline samples for route targeting, then calculates the eclipse at individual coordinates instead of treating a drawn path edge as perfectly exact.

~258 km

Maximum path width

Near greatest eclipse, NASA gives a path width of about 257.7 km.

6m 23s

Longest central duration

Maximum central totality is just over six minutes and twenty-three seconds.

1–3 km

Edge uncertainty

Lunar mountains and valleys can shift the predicted limit, which is why the site avoids edge-hugging recommendations.

Central totality duration along the 2027 path

Reduced NASA-derived centerline samples. The peak sits near southern Egypt before duration gradually declines farther east.

Central totality duration along the 2027 pathReduced NASA-derived centerline samples. The peak sits near southern Egypt before duration gradually declines farth3m 00s3m 48s4m 36s5m 24s6m 12s7m 00s08:263m 25s08:585m 18s09:306m 09s10:026m 23s10:346m 07s11:065m 24s11:384m 08s11:463m 33s
Central-line duration changes along the path. This chart describes the NASA-derived reduced centerline series, not the duration at every nearby town.

How the path of totality works

Totality is only visible inside a narrow corridor where the Moon fully covers the Sun's bright photosphere. The centerline runs through the middle of that corridor and generally provides longer totality than locations near an edge. But the centerline is not automatically the best real-world observing site because weather, access and mobility also matter.

Why Eclipse Wayfinder does not use a simple polygon edge as truth

NASA publishes northern and southern limits plus a central line at regular time intervals. Those limits are high-quality predictions, but the lunar limb is not a smooth circle. Mountains and valleys on the Moon change the exact moment and location where totality begins or ends. The site therefore uses centerline geometry to find a search direction and then checks local eclipse type directly with the astronomy engine.

Selected centerline samples

The table is a reduced set for readability. It shows how latitude, longitude, path width and central duration evolve along the event.

UTCLatitudeLongitudePath widthCentral totality
08:2630.4883°-36.2333°213 km3m 25s
08:4635.6600°-6.7217°236 km4m 48s
09:0635.0733°7.5550°246 km5m 34s
09:2632.8200°17.9067°252 km6m 04s
09:4629.5850°26.0967°255 km6m 20s
10:0625.6383°32.9800°258 km6m 23s
10:2621.0850°39.1667°259 km6m 14s
10:4615.9117°45.2250°258 km5m 54s
11:069.9717°51.8967°256 km5m 24s
11:262.7983°60.6767°248 km4m 42s
11:46-8.3067°79.5200°220 km3m 33s

Why you should not plan from the path edge

The edge is useful for geometry, not for an observing target. Small model differences, coordinate errors and lunar-limb effects can move the true limit enough to turn a barely-total site into a partial site. The Totality Finder therefore gives both a boundary estimate and a separate point 5 km farther inside the path.

Centerline versus best viewing location

Travelling all the way to the centerline may add only a small amount of totality once you are already deep inside the path. Use the Totality Gain Calculator to see where diminishing returns begin, then compare climate and practical factors.

Explore the path by destination

Western options include Málaga, Gibraltar and Tangier. Farther east, Luxor sits close to the longest-duration section, while Jeddah offers a different access profile.

Source

NASA GSFC: Total Solar Eclipse of 2027 August 2 — path table.