| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | August 27, 2045 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | 1.2060 | ||||||||
| Magnitude | −0.3899 | ||||||||
| Saros cycle | 148 (5 of 70) | ||||||||
| Penumbral | 241 minutes, 40 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sdescending node of orbit on Sunday, August 27, 2045,[1] with an umbralmagnitude of −0.3899. 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 1.6 days afterapogee (on August 26, 2045, at 0:10 UTC), the Moon's apparent diameter will be smaller.[2]
The eclipse will be completely visible overeast Asia andAustralia, seen rising overeast Africa andwest,central, andsouth Asia and setting over westernNorth America.[3]
 |
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Parameter | Value |
|---|---|
| Penumbral Magnitude | 0.68449 |
| Umbral Magnitude | −0.38987 |
| Gamma | 1.20606 |
| Sun Right Ascension | 10h26m15.1s |
| Sun Declination | +09°46'56.3" |
| Sun Semi-Diameter | 15'49.9" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 22h24m15.1s |
| Moon Declination | -08°48'49.2" |
| Moon Semi-Diameter | 14'44.1" |
| Moon Equatorial Horizontal Parallax | 0°54'04.7" |
| ΔT | 82.4 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.
| August 12 Descending node (new moon) | August 27 Ascending node (full moon) |
|---|---|
 | |
| Total solar eclipse Solar Saros 136 | Penumbral lunar eclipse Lunar Saros 148 |
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 | |
This eclipse is a part ofSaros series 148, repeating every 18 years, 11 days, and containing 70 events. The series started with a penumbral lunar eclipse onJuly 15, 1973. It contains partial eclipses from October 10, 2117 through May 5, 2460; total eclipses from May 17, 2478 through September 14, 2676; and a second set of partial eclipses from September 25, 2694 through May 25, 3091. The series ends at member 70 as a penumbral eclipse on August 9, 3217.
The longest duration of totality will be produced by member 37 at 104 minutes, 29 seconds on July 10, 2568. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series will occur on2568 Jul 10, lasting 104 minutes, 29 seconds.[7] | Penumbral | Partial | Total | Central |
1973 Jul 15 | 2117 Oct 10 | 2478 May 25 | 2514 Jun 08 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2622 Aug 13 | 2676 Sep 14 | 3091 May 25 | 3217 Aug 09 | |
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 1–13 occur between 1973 and 2200: | |||||
|---|---|---|---|---|---|
| 1 | 2 | 3 | |||
| 1973 Jul 15 | 1991 Jul 26 | 2009 Aug 06 | |||
|  |  |  |  |  |
| 4 | 5 | 6 | |||
| 2027 Aug 17 | 2045 Aug 27 | 2063 Sep 07 | |||
 |  | | | ||
| 7 | 8 | 9 | |||
| 2081 Sep 18 | 2099 Sep 29 | 2117 Oct 10 | |||
 |  | ||||
| 10 | 11 | 12 | |||
| 2135 Oct 22 | 2153 Nov 01 | 2171 Nov 12 | |||
| 13 | |||||
| 2189 Nov 22 | |||||
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 2132 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1805 Jul 11 (Saros 126) | 1816 Jun 10 (Saros 127) | 1827 May 11 (Saros 128) | 1838 Apr 10 (Saros 129) | 1849 Mar 09 (Saros 130) | |||||
| 1860 Feb 07 (Saros 131) | 1871 Jan 06 (Saros 132) | 1881 Dec 05 (Saros 133) | 1892 Nov 04 (Saros 134) | 1903 Oct 06 (Saros 135) | |||||
 |  | ||||||||
| 1914 Sep 04 (Saros 136) | 1925 Aug 04 (Saros 137) | 1936 Jul 04 (Saros 138) | 1947 Jun 03 (Saros 139) | 1958 May 03 (Saros 140) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1969 Apr 02 (Saros 141) | 1980 Mar 01 (Saros 142) | 1991 Jan 30 (Saros 143) | 2001 Dec 30 (Saros 144) | 2012 Nov 28 (Saros 145) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2023 Oct 28 (Saros 146) | 2034 Sep 28 (Saros 147) | 2045 Aug 27 (Saros 148) | 2056 Jul 26 (Saros 149) | 2067 Jun 27 (Saros 150) | |||||
 |  |  |  | | |  |  | ||
| 2132 Dec 22 (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 | |||||
|---|---|---|---|---|---|
| 1814 Feb 04 (Saros 140) | 1843 Jan 16 (Saros 141) | 1871 Dec 26 (Saros 142) | |||
| 1900 Dec 06 (Saros 143) | 1929 Nov 17 (Saros 144) | 1958 Oct 27 (Saros 145) | |||
 |  |  |  | ||
| 1987 Oct 07 (Saros 146) | 2016 Sep 16 (Saros 147) | 2045 Aug 27 (Saros 148) | |||
 |  |  |  | | |
| 2074 Aug 07 (Saros 149) | 2103 Jul 19 (Saros 150) | 2132 Jun 28 (Saros 151) | |||
| 2161 Jun 08 (Saros 152) | 2190 May 19 (Saros 153) | ||||
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 155.
| August 21, 2036 | September 2, 2054 |
|---|---|
 |  |
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