Figure 1 is an orthographic projection map of Earth [adapted from Espenak,
1987] showing the path of penumbral (partial) and umbral (total) eclipse. The
daylight terminator is plotted for the instant of greatest eclipse with north
at the top. The sub-Earth point is centered over the point of greatest eclipse
and is marked at **GE** with an asterisk. Earth's sub-solar point at that
instant is also indicated by the label **SS**.

The limits of the Moon's penumbral shadow delineate the region of visibility
of the partial solar eclipse. This irregular or saddle shaped region often
covers more than half of the daylight hemisphere of Earth and consists of
several distinct zones or limits. At the northern and/or southern boundaries
lie the limits of the penumbra's path. Partial eclipses have only one of these
limits, as do central eclipses when the shadow axis falls no closer than about
0.45 radii from Earth's center. Great loops at the western and eastern
extremes of the penumbra's path identify the areas where the eclipse
begins/ends at sunrise and sunset, respectively. If the penumbra has both a
northern and southern limit, the rising and setting curves form two separate,
closed loops. Otherwise, the curves are connected in a distorted figure eight.
Bisecting the 'eclipse begins/ends at sunrise and sunset' loops is the curve of
maximum eclipse at sunrise (western loop) and sunset (eastern loop). The
exterior tangency points **P1** and **P4** mark the coordinates where the
penumbral shadow first contacts (partial eclipse begins) and last contacts
(partial eclipse ends) Earth's surface. If the penumbral path has both a
northern and southern limit (as does the November 1994 eclipse), then the
interior tangency points **P2** and **P3** are also plotted and
correspond to the coordinates where the penumbral cone becomes internally
tangent to Earth's disk. Likewise, the points **U1** and **U2** mark the
exterior and interior coordinates where the umbral shadow initially contacts
Earth (path of total eclipse begins). The points **U3** and **U4** mark
the interior and exterior positions of the umbra's final contact with Earth's
surface (path of total eclipse ends).

A curve of maximum eclipse is the locus of all points where the eclipse is at maximum at a given time. Curves of maximum eclipse are plotted at each half hour Universal Time (UT). They generally run from the northern to the southern penumbral limits, or from the maximum eclipse at sunrise and sunset curves to one of the limits. The outline of the umbral shadow is plotted every ten minutes in UT. The curves of constant eclipse magnitude[2] delineate the locus of all points where the magnitude at maximum eclipse is constant. These curves run exclusively between the curves of maximum eclipse at sunrise and sunset. Furthermore, they are parallel to the northern/southern penumbral limits and the umbral paths of central eclipses. The northern and southern limits of the penumbra may be thought of as curves of constant magnitude of 0%. The adjacent curves are for magnitudes of 20%, 40%, 60% and 80%. The northern and southern limits of the path of total eclipse are curves of constant magnitude of 100%.

At the top of Figure 1, the Universal Time of geocentric conjunction between the Sun and Moon is given followed by the instant of greatest eclipse. The eclipse magnitude is given for greatest eclipse. For central eclipses (both total and annular), it is equivalent to the geocentric ratio of diameters of the Moon and the Sun. Gamma is the minimum distance of the Moon's shadow axis from Earth's center in units of equatorial Earth radii. The shadow axis passes south of Earth's geocenter for negative values of Gamma.

Finally, the extrapolated value of [[Delta]]T[3] used in the calculations is given.

[2] Eclipse magnitude is defined as the fraction or percentage of the Sun's diameter occulted by the Moon. It's usually expressed at greatest eclipse. Eclipse magnitude is strictly a ratio of

[3] [[Delta]]T is the difference between Terrestrial Dynamical Time and Universal Time