In August 1982, the International Astronomical Union (IAU) General Assembly adopted a value
of *k*=0.2725076 for the mean lunar radius. This value is now used by the Nautical Almanac Office for all
solar eclipse predictions [Fiala and Lukac, 1983] and is currently the best mean radius, averaging mountain
peaks and low valleys along the Moon's rugged limb. The adoption of one single value for
*k* eliminates the discontinuity in the case of annular-total eclipses and ends confusion arising from the use of two different
values. However, the use of even the best 'mean' value for the Moon's radius introduces a problem in predicting
the true character and duration of umbral eclipses, particularly total eclipses. A total eclipse can be defined as
an eclipse in which the Sun's disk is completely occulted by the Moon. This cannot occur so long as
any photospheric rays are visible through deep valleys along the Moon's limb [Meeus, Grosjean and
Vanderleen, 1966]. But the use of the IAU's mean
*k* guarantees that some annular or annular-total eclipses will
be misidentified as total. A case in point is the eclipse of 3 October 1986. Using the IAU value for
*k*, the *Astronomical Almanac* identified this event as a total eclipse of 3 seconds duration when it was, in fact,
a beaded annular eclipse. Since a smaller value of
*k* is more representative of the deeper lunar valleys
and hence the minimum solid disk radius, it helps ensure the correct
identification of an eclipse's true nature.

Of primary interest to most observers are the times when umbral eclipse begins and ends
(second and third contacts, respectively) and the duration of the umbral phase. When the IAU's value for
*k* is used to calculate these times, they must be corrected to accommodate low valleys (total) or high mountains
(annular) along the Moon's limb. The calculation of these corrections is not trivial but must be performed,
especially if one plans to observe near the path limits [Herald, 1983]. For observers near the center line of a
total eclipse, the limb corrections can be more closely approximated by using a smaller value of
*k* which accounts for the valleys along the profile.

This publication uses the IAU's accepted value of
*k*=0.2725076 for all penumbral (exterior)
contacts. In order to avoid eclipse type misidentification and to predict central durations which are closer to
the actual durations at total eclipses, we depart from standard convention by adopting the smaller value
of *k*=0.272281 for all umbral (interior) contacts. This is consistent with predictions in
*Fifty Year Canon of Solar Eclipses: 1986 -
2035* [Espenak, 1987]. Consequently, the smaller
*k* produces shorter umbral durations and narrower paths for total eclipses when compared with calculations using the IAU value for
*k*. Similarly, predictions using a smaller
*k* result in longer umbral durations and wider paths for annular eclipses than
do predictions using the IAU's *k*.

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