| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | March 3, 2045 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | −1.0274 | ||||||||
| Magnitude | −0.0148 | ||||||||
| Saros cycle | 143 (19 of 72) | ||||||||
| Penumbral | 243 minutes, 57 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sdescending node of orbit on Friday, March 3, 2045,[1] with an umbralmagnitude of −0.0148. A lunar eclipse occurs when theMoon moves into theEarth's shadow, causing the Moon to be darkened. A penumbral lunar eclipse occurs when part or all of the Moon's near side passes into the Earth's penumbra. Unlike asolar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on thenight side of Earth. Occurring about 1.8 days afterperigee (on March 1, 2045, at 13:40 UTC), the Moon's apparent diameter will be larger.[2]
The eclipse will be completely visible overNorth andSouth America, seen rising overnortheast Asia and easternAustralia and setting overwest Africa andwestern Europe.[3]
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Shown below is a table displaying details about this particular lunar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Parameter | Value |
|---|---|
| Penumbral Magnitude | 0.96431 |
| Umbral Magnitude | −0.01482 |
| Gamma | −1.02738 |
| Sun Right Ascension | 22h57m49.1s |
| Sun Declination | -06°37'35.6" |
| Sun Semi-Diameter | 16'08.1" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 10h55m51.5s |
| Moon Declination | +05°42'46.0" |
| Moon Semi-Diameter | 16'28.7" |
| Moon Equatorial Horizontal Parallax | 1°00'28.6" |
| ΔT | 82.1 s |
This eclipse is part of aneclipse season, a period, roughly every six months, when eclipses occur. Only two (or occasionally three) eclipse seasons occur each year, and each season lasts about 35 days and repeats just short of six months (173 days) later; thus two full eclipse seasons always occur each year. Either two or three eclipses happen each eclipse season. In the sequence below, each eclipse is separated by afortnight.
| February 16 Ascending node (new moon) | March 3 Descending node (full moon) |
|---|---|
 | |
| Annular solar eclipse Solar Saros 131 | Penumbral lunar eclipse Lunar Saros 143 |
This eclipse is a member of asemester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternatingnodes of the Moon's orbit.[5]
The penumbral lunar eclipse onOctober 28, 2042 occurs in the previous lunar year eclipse set.
| Lunar eclipse series sets from 2042 to 2045 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 113 | 2042 Apr 05 | Penumbral | 1.1080 | 118 | 2042 Sep 29 | Penumbral | −1.0261 | |
| 123 | 2043 Mar 25 | Total | 0.3849 | 128 | 2043 Sep 19 | Total | −0.3316 | |
| 133 | 2044 Mar 13 | Total | −0.3496 | 138 | 2044 Sep 07 | Total | 0.4318 | |
| 143 | 2045 Mar 03 | Penumbral | −1.0274 | 148 | 2045 Aug 27 | Penumbral | 1.2060 | |
TheMetonic cycle repeats nearly exactly every 19 years and represents aSaros cycle plus one lunar year. Because it occurs on the same calendar date, the Earth's shadow will be in nearly the same location relative to the background stars.
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This eclipse is a part ofSaros series 143, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on August 18, 1720. It contains partial eclipses fromMarch 14, 2063 through June 21, 2225; total eclipses from July 2, 2243 through April 13, 2712; and a second set of partial eclipses from April 25, 2730 through July 9, 2856. The series ends at member 72 as a penumbral eclipse on October 5, 3000.
The longest duration of totality will be produced by member 36 at 99 minutes, 9 seconds on September 6, 2351. All eclipses in this series occur at the Moon’sdescending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series will occur on2351 Sep 06, lasting 99 minutes, 9 seconds.[7] | Penumbral | Partial | Total | Central |
| 1720 Aug 18 | 2063 Mar 14 | 2243 Jul 02 | 2297 Aug 03 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2495 Dec 02 | 2712 Apr 13 | 2856 Jul 09 | 3000 Oct 05 | |
Eclipses are tabulated in three columns; every third eclipse in the same column is oneexeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
| Series members 6–27 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 6 | 7 | 8 | |||
| 1810 Oct 12 | 1828 Oct 23 | 1846 Nov 03 | |||
| 9 | 10 | 11 | |||
| 1864 Nov 13 | 1882 Nov 25 | 1900 Dec 06 | |||
| 12 | 13 | 14 | |||
| 1918 Dec 17 | 1936 Dec 28 | 1955 Jan 08 | |||
 |  |  |  |  |  |
| 15 | 16 | 17 | |||
| 1973 Jan 18 | 1991 Jan 30 | 2009 Feb 09 | |||
 |  |  |  |  |  |
| 18 | 19 | 20 | |||
| 2027 Feb 20 | 2045 Mar 03 | 2063 Mar 14 | |||
 |  | | | ||
| 21 | 22 | 23 | |||
| 2081 Mar 25 | 2099 Apr 05 | 2117 Apr 16 | |||
 |  | ||||
| 24 | 25 | 26 | |||
| 2135 Apr 28 | 2153 May 08 | 2171 May 19 | |||
| 27 | |||||
| 2189 May 29 | |||||
This eclipse is a part of atritos cycle, repeating at alternating nodes every 135synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.
| Series members between 1801 and 2187 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1805 Jan 15 (Saros 121) | 1815 Dec 16 (Saros 122) | 1826 Nov 14 (Saros 123) | 1837 Oct 13 (Saros 124) | 1848 Sep 13 (Saros 125) | |||||
| 1859 Aug 13 (Saros 126) | 1870 Jul 12 (Saros 127) | 1881 Jun 12 (Saros 128) | 1892 May 11 (Saros 129) | 1903 Apr 12 (Saros 130) | |||||
 |  | ||||||||
| 1914 Mar 12 (Saros 131) | 1925 Feb 08 (Saros 132) | 1936 Jan 08 (Saros 133) | 1946 Dec 08 (Saros 134) | 1957 Nov 07 (Saros 135) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1968 Oct 06 (Saros 136) | 1979 Sep 06 (Saros 137) | 1990 Aug 06 (Saros 138) | 2001 Jul 05 (Saros 139) | 2012 Jun 04 (Saros 140) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2023 May 05 (Saros 141) | 2034 Apr 03 (Saros 142) | 2045 Mar 03 (Saros 143) | 2056 Feb 01 (Saros 144) | 2066 Dec 31 (Saros 145) | |||||
 |  |  |  | | |  |  | ||
| 2077 Nov 29 (Saros 146) | 2088 Oct 30 (Saros 147) | 2099 Sep 29 (Saros 148) | 2110 Aug 29 (Saros 149) | 2121 Jul 30 (Saros 150) | |||||
 |  | ||||||||
| 2132 Jun 28 (Saros 151) | 2143 May 28 (Saros 152) | 2154 Apr 28 (Saros 153) | |||||||
| 2187 Jan 24 (Saros 156) | |||||||||
This eclipse is a part of the long periodinex cycle, repeating at alternating nodes, every 358synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic month (period of perigee). However, groupings of 3 inex cycles (≈ 87 years minus 2 months) comes close (≈ 1,151.02 anomalistic months), so eclipses are similar in these groupings.
| Series members between 1801 and 2200 | |||||
|---|---|---|---|---|---|
| 1813 Aug 12 (Saros 135) | 1842 Jul 22 (Saros 136) | 1871 Jul 02 (Saros 137) | |||
| 1900 Jun 13 (Saros 138) | 1929 May 23 (Saros 139) | 1958 May 03 (Saros 140) | |||
 |  |  |  | ||
| 1987 Apr 14 (Saros 141) | 2016 Mar 23 (Saros 142) | 2045 Mar 03 (Saros 143) | |||
 |  |  |  | | |
| 2074 Feb 11 (Saros 144) | 2103 Jan 23 (Saros 145) | 2132 Jan 02 (Saros 146) | |||
| 2160 Dec 13 (Saros 147) | 2189 Nov 22 (Saros 148) | ||||
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (ahalf saros).[8] This lunar eclipse is related to two partial solar eclipses ofSolar Saros 150.
| February 27, 2036 | March 9, 2054 |
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