This page is based on information published in the Five Millennium Canon of Lunar Eclipses: -1999 to +3000 and the Five Millennium Catalog of Lunar Eclipses: -1999 to +3000.

1.1 Statistical Distribution of Lunar Eclipse Types

Eclipses of the Moon can only occur during the Full Moon phase. It is then possible for the Moon to pass through Earth’s penumbral and umbral shadows thereby producing an eclipse. There are three types of lunar eclipses:

1. Penumbral – Moon passes partially or completely into Earth’s penumbral shadow.
2. Partial – Moon passes partially into Earth’s umbral shadow.
3. Total – Moon passes completely into Earth’s umbral shadow.

During the 5,000-year period from –1999 to +3000 (2000 BCE to 3000 CE [1]), Earth will experience 12,064 eclipses of the Moon. The statistical distribution of the three eclipse types over this interval is shown in Table 1.

During most penumbral eclipses, only part of the Moon passes through Earth’s penumbral shadow. Examples of such partial penumbral eclipses include: 2009 Feb 09, 2009 Jul 07, 2009 Aug 06, and 2012 Nov 28. However, it is also possible to have a penumbral eclipse in which the Moon passes completely within Earth’s penumbral shadow without entering the inner umbral shadow. Such total penumbral eclipses are quite rare compared to normal (or partial) penumbral eclipses. During the 21st century, there are 87 partial penumbral eclipses, but only 5 total penumbral eclipses: 2006 Mar 14, 2053 Aug 29, 2070 Apr 25, 2082 Aug 08, and 2099 Sep 29. Table 2 shows the distribution of the two penumbral eclipse types during the period covered by the Canon of Lunar Eclipses. For more on total penumbral eclipses, see Section 1.11.

Total lunar eclipses through Earth’s umbral shadow can be categorized as:

1. Central – The Moon passes through the central axis of Earth’s umbral shadow.
2. Non-Central – The Moon misses the central axis of Earth’s umbral shadow.

Using the above categories, the distribution of the 3,479 total eclipses is shown in Table 3.

Examples of central total eclipses include: 2000 Jul 16, 2011 Jun 15, 2018 Jul 27, and 2022 May 16. Several examples of non-central total eclipses are: 2010 Dec 21, 2011 Dec 10, 2014 Apr 15, and 2014 Oct 08.

Footnotes

[1] The terms BCE and CE are abbreviations for "Before Common Era" and "Common Era," respectively. They are the secular equivalents to the BC and AD dating conventions. (See: Year Dating Conventions)

1.2 Distribution of Lunar Eclipse Types by Century

Table 4 summarizes 5,000 years of eclipses by eclipse type over 100-year intervals. The average century contains 241 lunar eclipses of which 88 are penumbral, 84 are partial and 70 are total. Individual centuries deviate from these mean values in interesting ways. For instance, the total number of eclipses in a century varies from a minimum of 225 (century beginning –0899) to a maximum of 259 (centuries beginning 1101 and 2801). The number of penumbral eclipses varies from 76 (century 0301) to 100 (century 2801), while the number of partial eclipses ranges from 54 (century –1599) to 102 (centuries –0699, 1101, and 2801). Finally, the number of total lunar eclipses per century varies from 57 (centuries 0001 and 2801) to 89 (century 0801). Note that century 2801 not only has the most number of eclipses (259), it also has the maximum number of penumbral (100) and partial (102) eclipses, but the minimum number of total eclipses (57).

The last column of Table 4 lists the number of total lunar eclipse tetrads per century. A tetrad is a grouping of four consecutive total lunar eclipses each separated by six lunations. Their frequency is quite variable with some centuries having 0 tetrads, while others may have as many as 8. For more on tetrads, see Section 1.16.

When the data in Table 4 is displayed graphically in Figure 1, other important relationships are revealed. The most apparent feature is a periodic oscillation in the number of all lunar eclipses (Figure 1a), as well as in the individual types. By inspection, the period is about 600 years. Using tables from von Oppolzer's Canon der Finsternisse (1887) the Dutch astronomer G. van den Bergh (1954) calculated a period of 586 years. By studying the distributions of tetrad eclipse groups (Section 1.16), Meeus derived an empirical expression showing that this period is slowly decreasing (Meeus 2004b). While its current value is actually 565 years, the period was 618 years in –1999 and it will decrease to 552 years by +3000. A theoretical study by T. Hughes (Hughes 2004) demonstrates that the period is caused by the eccentricity of Earth’s orbit, which is gradually decreasing.

There are other interesting features in Figure 1. For instance, the number of total lunar eclipses as well as deep central total eclipses is highest when the number of all lunar eclipses is at a minimum. In contrast, numbers of penumbral eclipses, partial eclipses and non-central total eclipses all appear to be synchronized with the overall number of lunar eclipses. Finally, the number of total penumbral eclipses, and total lunar eclipse tetrads are most frequent during epochs when the overall number of lunar eclipses is at a minimum.

Figure 1 Lunar Eclipse Types by Century
(click for larger figure)

1.3 Distribution of Lunar Eclipse Types by Month

Table 5 summarizes 5,000 years of eclipses by eclipse type in each month of the year. The first value in each column is the number of eclipses of a given type for the corresponding month. The second value, in square brackets [ ], is the number of eclipses divided by the number of days in that month. This normalization allows direct comparison of eclipse frequencies in different months.

A brief examination of the normalized values in the column “Number of All Lunar Eclipses” shows that eclipses are equally distributed around the year. The same holds true for partial eclipses; however, the columns for penumbral and total eclipses reveal something interesting. Penumbral eclipses are about 6% more likely during the period of December– January–February compared to the months June–July–August. This effect is attributed to Earth’s elliptical orbit. Earth currently reaches perihelion in early January and aphelion in early July. Consequently, the Sun’s apparent diameter varies from 1,952 to 1,887 arcsec between perihelion and aphelion. The Sun’s larger apparent diameter at perihelion makes Earth’s penumbral shadow larger so penumbral eclipses are more frequent at that time.

The opposite argument holds true for total eclipses that are about 4% more likely during the period April to August, compared to the months November to February. In this case, the Sun’s smaller apparent size around aphelion increases the diameter of Earth’s umbral shadow so the frequency of total eclipses is slightly higher at that time.

1.4 Lunar Eclipse Frequency and the Calendar Year

There are 2 to 5 lunar eclipses in every calendar year. Table 6 shows the distribution in the number of eclipses per year for the 5,000 years covered in the Canon of Lunar Eclipses.

When two eclipses occur in one calendar year, they can be in any combination of N, P, or T (penumbral, partial, or total, respectively). Figure 7 lists the frequency of each eclipse combination, along with five recent years when the combination occurs. The table makes no distinction in the order of any two eclipses. For example, the eclipse combination PT includes all years where the order is either PT or TP.

Over 71% of all years containing two eclipses are composed of the combinations PP (34.2%) or TT (37.2%). The NT pair is the rarest combination with only six instances, all within the first two millennia of the Canon of Lunar Eclipses, and with five of the six involving a total penumbral eclipse.

a - N = Penumbral, P = Partial, and T = Total.
b - When years are surrounded by square brackets [ ], there are no other examples outside this range.

When three eclipses occur in one calendar year, there are nine possible combinations of N, P, or T. Figure 8 lists the frequency of each eclipse combination along with five recent years when each combination occurs. The table makes no distinction in the order of eclipses in any combination. For example, the eclipse combination NPT includes all years where the order is NPT, NTP, PNT, PTN, TPN, and TNP. The rarest combinations–NNT and NTT–each occurs six times or less in the five-millennium span of this work. Interestingly, no PPP combinations occur.

a - N = Penumbral, P = Partial, and T = Total.
b - When a year is bounded by a square bracket “[” or “]”, there are no other examples beyond that year.

When four eclipses occur in one calendar year, there are three possible combinations of eclipse types N, P, and T. Figure 9 lists the frequency of each eclipse combination along with five recent years when each combination occurs. The table makes no distinction in the order of eclipses in the seven combinations. The rarest combination NNPP occurs just 32 times.

a - N = Penumbral, P = Partial, and T = Total.
b - When a year is bounded by a square bracket “[” or “]”, there are no other examples beyond that year.

The maximum number of five lunar eclipses in one calendar year is quite rare. Over the 5,000-year span of the Canon of Lunar Eclipses, there are only 33 years containing five lunar eclipses. They occur in two possible combinations of eclipse types where four out of the five eclipses are always of type N. The first eclipse of such a quintet always occurs in the first half of January, while the last eclipse falls in the latter half of December. Figure 10 lists the frequency of the two eclipse combinations, along with recent years when each combination occurs. The rarest combination NNNPP (actually either PNPNN or NNPNP) occurred just three times. Once again, the table makes no distinction in the order of eclipses in any combination.

a - N = Penumbral, P = Partial, and T = Total.
b - When years are surrounded by square brackets [ ], there are no other examples outside this range.

1.5 Extremes in Eclipse Magnitude – Penumbral Lunar Eclipses

The penumbral eclipse magnitude is defined as the fraction of the Moon’s diameter immersed in Earth’s penumbral shadow. It is a unitless parameter that can be expressed numerically by

                                          Mp = xp/dm,                                     (1)

where Mp is the penumbral eclipse magnitude, dm is the apparent diameter of the Moon, and xp is the distance measured from the edge of the penumbral shadow to the edge of the Moon deepest in the penumbra.

The penumbral eclipse magnitude reaches its maximum value at the instant of greatest eclipse. This is the value shown in the figures in the Canon of Lunar Eclipses. A search through the 12,064 eclipses in the Canon of Lunar Eclipses reveals some interesting cases involving extreme values of the penumbral eclipse magnitude.

Seven penumbral eclipses have a maximum magnitude less than 0.0020 (Table 11). These events are all the first or last members in a Saros series. The smallest magnitude was the penumbral eclipse of –0780 Dec 13 with a magnitude of just 0.0004.

Table 12 lists the nine penumbral eclipses having a maximum magnitude greater than 1.0800. The greatest penumbral eclipse occurred on 1322 Nov 24 with a maximum magnitude of 1.0951. Because the penumbral magnitudes of these eclipses are all greater than 1, they are classified as total penumbral eclipses, i.e., the Moon is completely immersed within the penumbral shadow.

1.6 Extremes in Eclipse Magnitude – Partial Eclipses

The umbral eclipse magnitude is defined as the fraction of the Moon’s diameter immersed in Earth’s umbral shadow. It is a unitless parameter that can be expressed numerically by

                                          Mu = xu/dm,                                     (2)

where Mu is the umbral eclipse magnitude, dm is the apparent diameter of the Moon, and xu is the distance measured from the edge of the umbral shadow to the edge of the Moon deepest in the umbra.

The umbral eclipse magnitude reaches its maximum value at the instant of greatest eclipse. This is the value shown in the figures in the Appendix. A search through the 12,064 eclipses in the Canon of Lunar Eclipses reveals some interesting cases involving extreme values of the umbral eclipse magnitude in partial and total lunar eclipses.

Eleven partial eclipses have a maximum magnitude (at greatest eclipse) less than or equal to 0.0020 (Table 13). The partial eclipse with the smallest magnitude (at greatest eclipse) occurred on 1553 Jul 25 and had a magnitude of just 0.0001.

Nine partial eclipses have a maximum magnitude (at greatest eclipse) greater than or equal to 0.9980 (Table 14). The partial eclipse with the largest magnitude (at greatest eclipse) occurred on –1972 Jun 27 with a magnitude of 0.9998.

1.7 Extremes in Eclipse Magnitude – Total Lunar Eclipses

Twelve total eclipses have a maximum magnitude less than or equal to 1.0020 (Table 15). The smallest magnitude was the total eclipse of 1529 Oct 17 with a value of just 1.0001 (note the upcoming total eclipse of 2015 Apr 04 and its magnitude of 1.0008). Because the Moon’s passage through the umbral shadow is so shallow, these events all have short total phases less than 7 min.

Eight total eclipses have a maximum magnitude greater than or equal to 1.8700. Their total phase durations all last 98 to 99 min and gamma values are all close to 0.0 indicating that the Moon passes centrally through the middle of the umbral shadow. These eclipses all take place when the Moon is near perigee–the time when the ratio of the Moon’s to umbra’s diameters is at maximum. The total eclipse with the largest magnitude (1.8821) occurs on 2756 Jun 05.

1.8 Greatest Duration – Penumbral Lunar Eclipses

Nine penumbral eclipses each have durations of 292 min or more. Because the penumbral eclipse magnitude of each of these events is greater than 1, they are all classified as total penumbral eclipses. Each eclipse in Table 17 occurs near lunar apogee and within several weeks of aphelion. Earth’s penumbra is then largest, while the Moon exhibits a small angular diameter and travels relatively slowly, thereby extending the length of the eclipse.

1.9 Greatest Duration – Partial Lunar Eclipses

Seven partial eclipses have durations of 209 min or more. All of these events occur with the Moon close to apogee so its slow trajectory through the umbra tends to prolong the partial phase.

1.10 Greatest Duration – Total Lunar Eclipses

Eighteen total eclipses have durations greater than or equal to 106 min. The most recent one was 2000 Jul 16, while the next is 2123 Jun 09. All of these eclipses occur near aphelion and with the Moon close to apogee. Consequently, the Moon has a small angular diameter coupled with a relatively slow orbital motion with respect to the umbra. Furthermore, the umbral shadow is largest when Earth is at aphelion. Such conditions prolong the Moon’s passage through the umbra to produce long total lunar eclipses (Meeus, 2002).

Earth’s tropical longitude of perihelion is currently increasing by 1.72° per century. This means that the date of aphelion occurred about 17 days earlier for each 1000 years backwards from the present. This too is reflected in the dates seen in Table 19.

1.11 Total Penumbral Lunar Eclipses

During most penumbral eclipses, only part of the Moon passes through Earth’s penumbral shadow. However, it is also possible to have a penumbral eclipse in which the entire Moon passes completely within Earth’s penumbral shadow without entering the inner umbral shadow. The geocentric apparent diameter of the Moon ranges from an extreme minimum of 1763.0 arcsec (apogee) to an extreme maximum of 2011.8 arcsec (perigee). The penumbral annulus formed by the zone between the outer edges of the penumbra and umbra also undergoes extremes ranging from 1887.7 arcsec (aphelion) to 1951.9 arcsec (perihelion). From these values, it is apparent that the Moon cannot fit entirely within the penumbral annulus when it is near perigee (Meeus, 1997). As a consequence of the restrictive geometry and conditions, total penumbral eclipses are quite rare and account for just 3.2%, or 141 out of 4378 penumbral eclipses in the Canon of Lunar Eclipses. Table 20 lists the dates of all 141 total penumbral eclipses.

The frequency of total penumbra䁬 eclipse varies considerably with time. If the 5,000-year period covered by the Canon of Lunar Eclipses is divided into 100-year intervals, the number of total penumbral eclipses per century varies from 0 to a maximum of 9 (Table 4). For instance, the number of total penumbral eclipses in centuries beginning in 1701, 1801, and 1901 are 0, 2, and 9, respectively. The number of total penumbral eclipses appears to be correlated with the number of total eclipses, as well as the number of tetrads per century, and inversely correlated with the overall number of all lunar eclipses per century. When a century has a relatively large number of lunar eclipses, it has fewer total lunar eclipses and few or no total penumbral lunar eclipses or tetrads (Figure 1).

1.12 Lunar Eclipse Duos

A duo is a pair of eclipses separated by one lunation (synodic month). Of the 12,064 eclipses in the Canon of Lunar Eclipses, 3,054 eclipses (25.3%) belong to a duo. One eclipse of a duo always passes north of Earth’s shadow axis, while the other eclipse passes to the south. In most cases, both eclipses in a duo are penumbral eclipses; however, there are 51 instances (3.3% of duos) in the Canon where one eclipse is penumbral and the other is partial. In each of these pairs, the penumbral magnitude of the penumbral eclipse is quite small, as is the umbral magnitude of the partial eclipse. The dates and eclipse combinations of all lunar eclipse duos are listed in Table 21.

1.13 Lunar Eclipses Duos in One Calendar Month

There are 57 instances where both members of an eclipse duo occur in one calendar month. In most cases, both eclipses in the duos are penumbral. In three instances, the duo consists of the NP combination (–1774 May, –0252 Jul, and 2960 Jun). The year and month of each duo appears in Table 22.

1.14 January–March Lunar Eclipse Duos

The mean length of one synodic month is 29.5306 days (in year 2000). Because this is longer than the month of February, it is possible to have one member of an eclipse duo in January followed by the second in March. There are six instances of such a rare January/March duo in the Canon of Lunar Eclipses: –1109, –0523, –0002, 1915, 2306, and 2371. In all cases, both eclipses in the duos are penumbral.

1.15 Total Lunar Eclipse Multiplets

A total lunar eclipse is usually preceded or succeeded by at least one other total lunar eclipse. Of the 3479 total eclipses in the Canon of Lunar Eclipses, 1798 of them (51.7%) are part of a doublet. Another 1023 eclipses (29.4%) belong to a triplet. Finally, 568 total eclipses (16.3%) are part of a quadruplet known as a tetrad. In comparison, only 90 total eclipses (2.6%) occur as solitary singlets.

A key feature of total lunar eclipse multiplets is that the individual members are always separated by six lunations. A summary of the muliplet statistics appears in Table 23.

1.16 Lunar Eclipse Tetrads

When four consecutive lunar eclipses are all total, the group is termed a tetrad. As discussed previously, 16.3% (568 out of 3479) of all total eclipses are members of a tetrad. These 142 groupings of total eclipses occur because of the eccentricity of Earth’s orbit in conjunction with the timing of eclipse seasons (Section 1.18). During the first 1,000 years of the Canon of Lunar Eclipses, the first eclipse of every tetrad occurs sometime from December to May. In later millennia, the first eclipse date occurs later in the year because of precession–during the 3rd Millennium, the period for the first date extends from February to July. For a detailed description of tetrad geometry and an explanation of why tetrads happen, see Meeus (2004b).

Italian astronomer Giovanni Schiaparelli first pointed out that the frequency of tetrads is variable over time. He noticed that tetrads were relatively plentiful during one 300-year interval, while none occurred during the next 300 years. For example, there are no tetrads from 1582 to 1908, but 17 tetrads occur during the following 2 1⁄2 centuries from 1909 to 2156. This can be seen graphically in Figure 1i. The 565-year period of the tetrad “seasons” is tied to the slowly decreasing eccentricity of Earth’s orbit. Consequently, the tetrad period is gradually decreasing (Hughes, 2004). In the distant future, when Earth’s eccentricity is 0, tetrads will no longer be possible.

The umbral magnitudes of the total eclipses making up a tetrad are all relatively small. For the 300-year period 1901 to 2200, the largest umbral magnitude of a tetrad eclipse is 1.4251 on 1949 Apr 13. For comparison, some other total eclipses during this period are much deeper. Two examples are the total eclipses of 2000 Jul 16 and 2029 Jun 26 with umbral magnitudes of 1.7684 and 1.8436, respectively.

Table 24 lists the date of the first total lunar eclipse in each of the 142 tetrads in the Canon of Lunar Eclipses.

1.17 Lunar Eclipses on February 29

There are six instances of a lunar eclipse occurring on February 29. Two eclipses are penumbral, two are partial, and two are total. A list of eclipses on February 29 with physical parameters appears in Table 25.

a - Penumbral Eclipse Magnitude

1.18 Eclipse Seasons

The 5.1° inclination of the lunar orbit around Earth means that the Moon’s orbit crosses the ecliptic at two points or nodes. If Full Moon takes place within about 16° of a node [2], then a lunar eclipse will be visible from a portion of Earth.

The Sun makes one complete circuit of the ecliptic in 365.24 days, so its average angular velocity is 0.99° per day. At this rate, it takes 34.5 days for Earth’s umbral and penumbral shadows to cross the 34° wide eclipse zone centered on each node. Because the Moon’s orbit with respect to the Sun has a mean duration of 29.53 days, there will always be one, and possibly two, lunar eclipses during each 34.5-day interval when the Sun (and Earth’s shadows) pass through the nodal eclipse zones. These time periods are called eclipse seasons.

The mid-point of each eclipse season is separated by 173.3 days because this is the mean time for the Sun to travel from one node to the next. The period is a little less than half a calendar year because the lunar nodes slowly regress westward by 19.3° per year.

Footnotes

[2] The actual value ranges from 15.2° to 16.8° because of the eccentricity of the Moon's and Earth's orbits. If a lunar eclipse occurs within 9.4° to 11.0° of a node, the eclipse will be partial. A lunar eclipse within 4.2° to 5.0°of a node will be total.

1.19 Quincena

The mean time interval between New Moon and Full Moon is 14.77 days. This is less than half the duration of an eclipse season. As a consequence, the same Sun–node alignment geometry responsible for producing a lunar eclipse always results in a complementary solar eclipse within a fortnight. The solar eclipse may either precede or succeed the lunar eclipse. In either case, the pair of eclipses is referred to here as a quincena. The Quincena Solar Eclipse (QSE) parameter identifies the type of the solar eclipse and whether it precedes or succeeds a particular lunar eclipse. There are four types of solar eclipses:

1. p = partial solar eclipse
   (Moon’s penumbral shadow traverses Earth; umbral/antumbral shadow completely misses Earth)
2. a = annular solar eclipse
   (Moon’s antumbral shadow traverses Earth; Moon is too far from Earth to completely cover the Sun)
3. t = total solar eclipse
   (Moon’sumbral shadow traverses Earth; Moon is close enough to Earth to completely cover the Sun)
4. h = hybrid solar eclipse
   (Moon’s umbral and antumbral shadows traverse different parts of Earth; eclipse appears either total or annular along different sections of its path–hybrid eclipses are also known as annular-total eclipses)

The QSE is a two character string consisting of one or more of the above solar eclipse types. The first character in the QSE identifies a solar eclipse preceding a lunar eclipse while the second character identifies a solar eclipse succeeding a lunar eclipse. In most instances, one of the two characters is “–” indicating a single solar eclipse either precedes or succeeds the lunar eclipse. On rare occasions, a double quincena occurs in which a lunar eclipse is both preceded and succeeded by solar eclipses.

1.20 Quincena Combinations with Total Lunar Eclipses

A total lunar eclipse can be preceded or succeeded by a total solar eclipse (7.7%), an annular solar eclipse (10.2%), a hybrid solar eclipse (0.4%), or a partial solar eclipse (42.5%). Double quincenas (a lunar eclipse is both preceded and succeeded by a solar eclipse) occur with a frequency of 39.1% and usually consist of two partial solar eclipses (38.7%). In rare instances, a double quincena consists of a total and a partial solar eclipse (0.4%). A complete list of all QSE combinations with total lunar eclipses appears in Table 26. The most recent years when each quincena combination occurs are given in the last column.

a - When a year is bounded by a square bracket “[” or “]”, there are no other examples beyond that year.

1.21 Quincena Combinations with Partial Lunar Eclipses

A partial lunar eclipse can be preceded or succeeded by a total solar eclipse (37.6%), an annular solar eclipse (55.1%), or a hybrid solar eclipse (6.9%). In rare instances, a partial lunar eclipse can be followed by a partial solar eclipse (0.3%). Double quincenas do not occur with partial lunar eclipses. A list of quincena solar eclipse combinations with partial lunar eclipses appears in Table 27. The most recent years when each quincena combination occurs are given in the last column.

a - When a year is bounded by a square bracket “[” or “]”, there are no other examples beyond that year.

1.22 Quincena Combinations with Penumbral Lunar Eclipses

A penumbral lunar eclipse can be preceded or succeeded by a total solar eclipse (39.5%), an annular solar eclipse (51.9%), or a hybrid solar eclipse (8.7%). There are no instances of a quincena involving a partial solar and a penumbral lunar eclipse, nor are there any double quincenas in the Canon of Lunar Eclipses. A list of quincena solar eclipse combinations with penumbral lunar eclipses appears in Table 28. The most recent years when each quincena combination occurs are given in the last column.

Acknowledgments

The information presented on this web page is based on material originally published in Five Millennium Canon of Lunar Eclipses: -1999 to +3000 and Five Millennium Catalog of Lunar Eclipses: -1999 to +3000. All eclipse calculations are by Fred Espenak, and he assumes full responsibility for their accuracy.

Permission is freely granted to reproduce this data when accompanied by an acknowledgment:

"Eclipse Predictions by Fred Espenak and Jean Meeus, www.EclipseWise.com"

The use of diagrams and maps is permitted provided that they are NOT altered (except for re-sizing) and the embedded credit line is NOT removed or covered.

References

Espenak, F., and Meeus, J., Five Millennium Canon of Lunar Eclipses: -1999 to +3000, Astropixels Publishing, Portal, AZ (2022).

Espenak, F., and Meeus, J., Five Millennium Catalog of Lunar Eclipses: -1999 to +3000, Astropixels Publishing, Portal, AZ (2022).

Gingerich, O., (Translator), Canon of Eclipses, Dover Publications, New York (1962) (from the original T.R. von Oppolzer, book, Canon der Finsternisse, Wien, [1887]).

Meeus, J., Mathematical Astronomy Morsels, Willmann-Bell, Richmond, Virginia, pp. 108–110, (1997).

Meeus, J., More Mathematical Astronomy Morsels, Willmann-Bell, Richmond, Virginia, pp. 120–126 (2002).

Meeus, J., Mathematical Astronomy Morsels III, Willmann-Bell, Richmond, Virginia, pp. 109–111, (2004a).

Meeus, J., Grosjean, C.C., and Vanderleen, W., Canon of Solar Eclipses, Pergamon Press, Oxford, United Kingdom (1966).

van den Bergh, G., Periodicity and Variation of Solar (and Lunar) Eclipses, Tjeenk Willink, and Haarlem, Netherlands (1955).

von Oppolzer, T.R., Canon der Finsternisse, Wien, (1887).

Relevant Links:

Six Millennium Catalog of Lunar Eclipses

Lunar Eclipse Statistics

Periodicity of Lunar Eclipses

Catalog of Lunar Eclipse Saros Series

Eclipses and the Moon's Orbit

Eclipses and the Saros

Six Millennium Catalog of Solar Eclipses

Solar Eclipse Statistics

Periodicity of Solar Eclipses

Catalog of Solar Eclipse Saros Series

Links to Additional Lunar Eclipse Predictions

• Home - home page of EclipseWise with predictions for both solar and lunar eclipses

• Lunar Eclipses - primary page for lunar eclipse predictions
• Lunar Eclipse Links - detailed directory of links

• Six Millennium Catalog of Lunar Eclipses - covers the years -2999 to +3000 (3000 BCE to 3000 CE)
• Javascript Lunar Eclipse Explorer - calculate all lunar eclipses visible from a city

• Five Millennium Canon of Lunar Eclipses: -1999 to +3000 - link to the publication
• Five Millennium Catalog of Lunar Eclipses: -1999 to +3000 - link to the publication
• Thousand Year Canon of Lunar Eclipses 1501 to 2500 - link to the publication

• MrEclipse.com - eclipse resources and tips on photography
• Lunar Eclipses for Beginners - a primer on lunar eclipse basics
• How to Photograph a Lunar Eclipse - instructions for imaging an eclipse of the Sun
• MrEclipse Photo Index - an index of lunar eclipse photographs

Lunar Eclipse Publications