Total penumbral lunar eclipse

A total penumbral eclipse is a lunar eclipse occurs when the moon becomes completely immersed in the penumbral cone of the Earth without touching the umbra. [1]

It is a narrow path for the moon to pass within the peumbral and outside the umbra. It can happen on the Earth's northern or southern penumbral edges. In addition size of the penumbral is sometimes too small to contain the moon. Its width is equal to the angular diameter of the sun at the time of the eclipse, and the moon's angular diameter is larger than the sun over part of its elliptical orbit, depending on whether the eclipse occurs at its nearest (perigee) or farthest point (apogee) in its orbit around the earth.

Contents

Frequency

This occurs in a relatively small fraction of lunar eclipses, and the distribution of these events is uneven, occurring between 0 and 9 times per century. The period of this variation is about 600 years and also correlates with the frequency of total umbral eclipses and tetrads.

Summary frequency 501–2500

Century Total
penumbral		 Total
umbral		 Tetrads
501–600 1 63 0
601–700 2 58 0
701–800 2 69 3
801–900 5 88 8
901–1000 3 78 6
1001–1100 3 62 0
1101–1200 0 60 0
1201–1300 1 60 0
1301–1400 8 77 6
1401–1500 4 83 4
1501–1600 2 76 6
1601–1700 2 61 0
1701–1800 0 60 0
1801–1900 2 62 0
1901–2000 9 81 5
2001–2100 5 84 7
2101–2200 5 69 4
2201–2300 1 61 0
2301–2400 0 60 0
2401–2500 6 69 4

List of events 1901–2100

Ascending nodes Descending nodes
Saros Date Viewing Chart Saros Date Viewing Chart
110 1901 May 03
114 1908 Dec 07
114 1926 Dec 19
114 1944 Dec 29
116 1948 Oct 18
114 1963 Jan 09
114 1981 Jan 20 113 1988 Mar 03
114 1999 Jan 31 113 2006 Mar 14
119 2053 Aug 29
142 2070 Apr 25
120 2082 Aug 08
148 2099 Sep 29

See also

Notes

  1. ^ Total Penumbral lunar eclipses, Jean Meeus, 1980