Table 6
provides topocentric data and corrections to the path limits due to the true lunar limb
profile. At five minute intervals, the table lists the Moon's topocentric horizontal parallax, semi-diameter,
relative angular velocity of the Moon with respect to the Sun and lunar libration in longitude. The Sun's
center line altitude and azimuth is given, followed by the azimuth of the umbral path. The position angle of
the point on the Moon's limb which defines the northern limit of the path is measured counter-clockwise
(*i.e.*, eastward) from the north point on the limb. The path corrections to the northern and southern limits are
listed as interior and exterior components in order to define the graze zone. Positive corrections are in the
northern sense while negative shifts are in the southern sense. These corrections (minutes of arc in latitude) may
be added directly to the path coordinates listed in
Table 3. Corrections
to the center line umbral durations due
to the lunar limb profile are also included and they are mostly positive. Thus, when added to the central
durations given in
Tables 3,
4,
5, and
7, a slightly longer
central total phase is predicted.

Detailed coordinates for the zones of grazing eclipse at each limit for all land based sections of the path are presented in Table 8. Given the uncertainties in the Watts data, these predictions should be accurate to ±0.3 arc-seconds. The interior graze coordinates take into account the deepest valleys along the Moon's limb which produce the simultaneous second and third contacts at the path limits. Thus, the interior coordinates define the true edge of the path of totality. They are calculated from an algorithm which searches the path limits for the extreme positions where no photospheric beads are visible along a ±30° segment of the Moon's limb, symmetric about the extreme contact points at the instant of maximum eclipse. The exterior graze coordinates are somewhat arbitrarily defined and calculated for the geodetic positions where an unbroken photospheric crescent of 60° in angular extent is visible at maximum eclipse.

In Table 8,
the graze zone latitudes are listed every 1° in longitude (at sea level) and include the
time of maximum eclipse at the northern and southern limits as well as the path's azimuth. To correct the path
for locations above sea level, *Elev Fact*^{8} is a
multiplicative factor by which the path must be shifted
north perpendicular to itself (*i.e.*, perpendicular to path azimuth) for each unit of elevation (height) above
sea level. To calculate the shift, a location's elevation is multiplied by the
*Elev Fact* value. Negative values (usually the case for eclipses in the Northern Hemisphere) indicate that the path must be shifted south.
For instance, if one's elevation is 1000 meters above sea level and the
*Elev Fact* value is 0.20, then the shift
is 200m (= 1000m x 0.20). Thus, the observer must shift the path coordinates 200 meters in a
direction perpendicular to the path and in a negative or southerly sense.

The final column of
Table 8
lists the
*Scale Fact* (km/arc-second). This scaling factor provides
an indication of the width of the zone of grazing phenomena, due to the topocentric distance of the Moon
and the projection geometry of the Moon's shadow on Earth's surface. Since the solar chromosphere has
an apparent thickness of about 3 arc-seconds, and assuming a
*Scale Fact* value of 2 km/arc-seconds, then
the chromosphere should be visible continuously during totality for any observer in the path who is within
6 kilometers (=2x3) of each interior limit. However, the most dynamic beading phenomena occurs within
1.5 arc-seconds of the Moon's limb. Using the above Scale Factor, this translates into the first 3
kilometers inside the interior limits. But observers should position themselves at least 1 kilometer inside the
interior limits (south of the northern interior limit or north of the southern interior limit) in order to ensure that
they are inside the path due of to small uncertainties in Watts' data and the
actual path limits.

For applications where the zones of grazing eclipse are needed at a higher frequency in longitude interval, tables of coordinates every 7.5' in longitude are available via a special Web site for the total solar eclipse of 1999 August 11.

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