The geocentric ephemeris for the Sun and Moon, various parameters, constants, and the Besselian elements (polynomial form) are given in Table 1. The eclipse elements and predictions were derived from the DE200 and LE200 ephemerides (solar and lunar, respectively) developed jointly by the Jet Propulsion Laboratory and the U. S. Naval Observatory for use in the Astronomical Almanac for 1984 and thereafter. Unless otherwise stated, all predictions are based on center of mass positions for the Moon and Sun with no corrections made for center of figure, lunar limb profile or atmospheric refraction. The predictions depart from normal IAU convention through the use of a smaller constant for the mean lunar radius k for all umbral contacts (see: Lunar Limb Profile). Times are expressed in either Terrestrial Dynamical Time (TDT) or in Universal Time (UT), where the best value of Delta T
From the polynomial form of the Besselian elements, any element can be evaluated for any time t_{1 } (in decimal hours) via the equation:
t = t_{1} Ð t_{0} (decimal hours) and t_{0} = 17.000 TDT
The polynomial Besselian elements were derived from a leastsquares fit to elements rigorously calculated at five separate times over a six hour period centered at t_{0}. Thus, the equation and elements are valid over the period 14.00 <= t_{0} <= 20.00 TDT.
Table 2 lists all external and internal contacts of penumbral and umbral shadows with Earth. They include TDT times and geodetic coordinates with and without corrections for Delta T. The contacts are defined:
P1  Instant of first external tangency of penumbral shadow cone with Earth's limb. (partial eclipse begins)
U1  Instant of first external tangency of umbral shadow cone with Earth's limb. (umbral eclipse begins)
U2  Instant of first internal tangency of umbral shadow cone with Earth's limb.
U3  Instant of last internal tangency of umbral shadow cone with Earth's limb.
U4  Instant of last external tangency of umbral shadow cone with Earth's limb. (umbral eclipse ends)
P4  Instant of last external tangency of penumbral shadow cone with Earth's limb. (partial eclipse ends)
Similarly, the northern and southern extremes of the penumbral and umbral paths, and extreme limits of the umbral center line are given. The IAU longitude convention is used throughout this publication (i.e., for longitude, east is positive and west is negative; for latitude, north is positive and south is negative).
The path of the umbral shadow is delineated at five minute intervals in Universal Time in Table 3. Coordinates of the northern limit, the southern limit and the center line are listed to the nearest tenth of an arcminute (~185 m at the Equator). The Sun's altitude, path width and umbral duration are calculated for the center line position. Table 4 presents a physical ephemeris for the umbral shadow at five minute intervals in UT. The center line coordinates are followed by the topocentric ratio of the apparent diameters of the Moon and Sun, the eclipse obscuration^{2}, and the Sun's altitude and azimuth at that instant. The central path width, the umbral shadow's major and minor axes and its instantaneous velocity with respect to Earth's surface are included. Finally, the center line duration of the umbral phase is given.
Local circumstances for each center line position listed in Tables 3 and 4 are presented in Table 5. The first three columns give the Universal Time of maximum eclipse, the center line duration of totality and the altitude of the Sun at that instant. The following columns list each of the four eclipse contact times followed by their related contact position angles and the corresponding altitude of the Sun. The four contacts identify significant stages in the progress of the eclipse. They are defined as follows:
First Contact  Instant of first external tangency between the Moon and Sun. (partial eclipse begins)
Second Contact  Instant of first internal tangency between the Moon and Sun. (central or umbral eclipse begins; total or annular eclipse begins)
Third Contact  Instant of last internal tangency between the Moon and Sun. (central or umbral eclipse ends; total or annular eclipse ends)
Fourth Contact  Instant of last external tangency between the Moon and Sun. (partial eclipse ends)
The position angles P and V identify the point along the Sun's disk where each contact occurs^{3}. Second and third contact altitudes are omitted since they are always within 1° of the altitude at maximum eclipse.
Table 6 presents topocentric values from the central path at maximum eclipse for the Moon's horizontal parallax, semidiameter, relative angular velocity with respect to the Sun, and libration in longitude. The altitude and azimuth of the Sun are given along with the azimuth of the umbral path. The northern limit position angle identifies the point on the lunar disk defining the umbral path's northern limit. It is measured counterclockwise from the north point of the Moon. In addition, corrections to the path limits due to the lunar limb profile are listed. The irregular profile of the Moon results in a zone of 'grazing eclipse' at each limit that is delineated by interior and exterior contacts of lunar features with the Sun's limb. This geometry is described in greater detail in the section Limb Corrections To The Path Limits: Graze Zones. Corrections to center line durations due to the lunar limb profile are also included. When added to the durations in Tables 3, 4, 5 and 7, a slightly longer central total phase is predicted along most of the path.
To aid and assist in the plotting of the umbral path on large scale maps, the path coordinates are also tabulated at 30' intervals in longitude in Table 7. The latitude of the northern limit, southern limit and center line for each longitude is tabulated to the nearest hundredth of an arcminute (~18.5 m at the Equator) along with the Universal Time of maximum eclipse at each position. Finally, local circumstances on the center line at maximum eclipse are listed and include the Sun's altitude and azimuth, the umbral path width and the central duration of totality.
In applications where the zones of grazing eclipse are needed in greater detail, Table 8 lists these coordinates over land based portions of the path at 15' intervals in longitude. The time of maximum eclipse is given at both northern and southern limits as well as the path's azimuth. The elevation and scale factors are also given (See: Limb Corrections To The Path Limits: Graze Zones).
^{1} Delta T is the difference between Terrestrial Dynamical Time and Universal Time.
^{2}Eclipse obscuration is defined as the fraction of the Sun's surface area occulted by the Moon.
^{3}P is defined as the contact angle measured counterclockwise from the north point of the Sun's disk.
V is defined as the contact angle measured counterclockwise from the zenith point of the Sun's disk.
Adapted from NASA RP 1398 "Total Solar Eclipse of 1998 February 26".
WebMaster: Fred Espenak Planetary Systems Branch  Code 693 email: espenak@lepvax.gsfc.nasa.gov NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771 USA

