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Total penumbral lunar eclipse
A total penumbral eclipse is a lunar eclipse that occurs when the moon becomes completely immersed in the penumbral cone of the Earth without touching the umbra.〔 (Total Penumbral lunar eclipses, Jean Meeus, 1980 ) 〕
It is a narrow path for the moon to pass within the penumbra and outside the umbra. It can happen on the Earth's northern or southern penumbral edges. In addition, the size of the penumbra is sometimes too small where the moon enters it to contain the moon. The width of the Earth's penumbra is determined by the sun's angular diameter 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. The majority of the time, the size of the moon and the size of the Earth's penumbra where the moon crosses it mean that most eclipses will not be total penumbral in nature.
== Frequency ==
Such eclipses constitute 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.
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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