Annular) 18 11 7 42
--------------------------------------------
(Mag. Annular) 1901 Nov. 11 7 19 a.m. (civil time) +1 m.

The foregoing does not by any means exhaust all that can be said
respecting the Saros even on the popular side.

If the Saros comprised an exact number of days, each eclipse of a second
Saros series would be visible in the same regions of the Earth as the
corresponding eclipse in the previous series. But since there is a
surplus fraction of nearly one-third of a day, each subsequent eclipse
will be visible in another region of the Earth, which will be roughly a
third of the Earth's circumference in longitude backwards (_i.e._ about
120 deg. to the W.), because the Earth itself will be turned on its axis
one-third forwards.

After what has been said as to the Saros and its use it might be
supposed that a correct list of eclipses for 18.03 years would suffice
for all ordinary purposes of eclipse prediction, and that the sequence
of eclipses at any future time might be ascertained by adding to some
one eclipse which had already happened so many Saros periods as might
embrace the years future whose eclipses it was desired to study. This
would be true in a sense, but would not be literally and effectively
true, because corresponding eclipses do not recur exactly under the same
conditions, for there are small residual discrepancies in the times and
circumstances affecting the real movements of the Earth and Moon and the
apparent movement of the Sun which, in the lapse of years and centuries,
accumulate sufficiently to dislocate what otherwise would be exact
coincidences. Thus an eclipse of the Moon which in A.D. 565 was of 6
digits[7] was in 583 of 7 digits, and in 601 nearly 8. In 908 the
eclipse became total, and remained so for about twelve periods, or until
1088. This eclipse continued to diminish until the beginning of the 15th
century, when it disappeared in 1413. Let us take now the life of an
eclipse of the Sun. One appeared at the North Pole in June A.D. 1295,
and showed itself more and more towards the S. at each subsequent
period. On August 27, 1367, it made its first appearance in the North of
Europe; in 1439 it was visible all over Europe; in 1601, being its 19th
appearance, it was central and annular in England; on May 5, 1818, it
was visible in London, and again on May 15, 1836. Its three next
appearances were on May 26, 1854, June 6, 1872, and June 17, 1890. At
its