| Total eclipse | |||||||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||||||
| Date | June 28, 2094 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | 0.0288 | ||||||||||||||||
| Magnitude | 1.8249 | ||||||||||||||||
| Saros cycle | 131 (38 of 72) | ||||||||||||||||
| Totality | 100 minutes, 36 seconds | ||||||||||||||||
| Partiality | 235 minutes, 42 seconds | ||||||||||||||||
| Penumbral | 326 minutes, 27 seconds | ||||||||||||||||
| |||||||||||||||||
← January 2094 December 2094 → | |||||||||||||||||
A totallunar eclipse will occur at the Moon’sdescending node of orbit on Monday, June 28, 2094,[1] with an umbralmagnitude of 1.8249. It will be acentral lunar eclipse, in which part of theMoon will pass through thecenter of theEarth's shadow. A lunar eclipse occurs when theMoon moves into theEarth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. 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. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon'sshadow is smaller. Occurring about 1.9 days beforeperigee (on June 30, 2094, at 7:50 UTC), the Moon's apparent diameter will be larger.[2]
While the visual effect of a total eclipse is variable, the Moon may be stained a deep orange or red color at maximum eclipse. With a gamma value of only 0.0288 and anumbral eclipse magnitude of 1.8249, this is the greatest eclipse inLunar Saros 131 as well as the second largest and darkest lunar eclipse of the21st century.
During the eclipse,NGC 6629 will be occulted by theMoon over NortheastAustralia and thePacific Ocean;NGC 6642 will be occulted by the Moon overNew Guinea,Northern Australia and the Pacific Ocean.Deep-sky objects are rarely occulted during a total eclipse from any given spot on Earth.[3]: 161
The eclipse will be completely visible over easternAustralia,Antarctica, and the central and easternPacific Ocean, seen rising overeast Asia and western Australia and setting overNorth andSouth America.[4]
 |
Shown below is a table displaying details about this particular lunar eclipse. It describes various parameters pertaining to this eclipse.[5]
| Parameter | Value |
|---|---|
| Penumbral Magnitude | 2.78793 |
| Umbral Magnitude | 1.82485 |
| Gamma | 0.02882 |
| Sun Right Ascension | 06h31m43.3s |
| Sun Declination | +23°13'34.7" |
| Sun Semi-Diameter | 15'44.1" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 18h31m43.6s |
| Moon Declination | -23°11'51.1" |
| Moon Semi-Diameter | 16'20.2" |
| Moon Equatorial Horizontal Parallax | 0°59'57.5" |
| ΔT | 121.4 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. The first and last eclipse in this sequence is separated by onesynodic month.
| June 13 Ascending node (new moon) | June 28 Descending node (full moon) | July 12 Ascending node (new moon) |
|---|---|---|
 | |  |
| Partial solar eclipse Solar Saros 119 | Total lunar eclipse Lunar Saros 131 | Partial solar eclipse Solar Saros 157 |
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.[6]
The penumbral lunar eclipses onFebruary 23, 2092 andAugust 17, 2092 occur in the previous lunar year eclipse set, and the penumbral lunar eclipses onMay 7, 2096 andOctober 31, 2096 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 2092 to 2096 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 111 | 2092 Jul 19 | Penumbral | 1.5131 | 116 | 2093 Jan 12 | Penumbral | −1.1733 | |
| 121 | 2093 Jul 08 | Partial | 0.7632 | 126 | 2094 Jan 01 | Partial | −0.5024 | |
| 131 | 2094 Jun 28 | Total | 0.0288 | 136 | 2094 Dec 21 | Total | 0.2016 | |
| 141 | 2095 Jun 17 | Partial | −0.7653 | 146 | 2095 Dec 11 | Partial | 0.8742 | |
| 151 | 2096 Jun 06 | Penumbral | −1.5723 | 156 | 2096 Nov 29 | Penumbral | 1.5017 | |
This eclipse is a part ofSaros series 131, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on May 10, 1427. It contains partial eclipses from July 25, 1553 throughMarch 22, 1932; total eclipses fromApril 2, 1950 through September 3, 2202; and a second set of partial eclipses from September 13, 2220 through April 9, 2563. The series ends at member 72 as a penumbral eclipse on July 7, 2707.
The longest duration of totality will be produced by member 38 at 100 minutes, 36 seconds onJune 28, 2094. All eclipses in this series occur at the Moon’sdescending node of orbit.[7]
| Greatest | First | |||
|---|---|---|---|---|
The greatest eclipse of the series will occur on2094 Jun 28, lasting 100 minutes, 36 seconds.[8] | Penumbral | Partial | Total | Central |
| 1427 May 10 | 1553 Jul 25 | 1950 Apr 02 | 2022 May 16 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2148 Jul 31 | 2202 Sep 03 | 2563 Apr 09 | 2707 Jul 07 | |
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 22–43 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 22 | 23 | 24 | |||
| 1806 Jan 05 | 1824 Jan 16 | 1842 Jan 26 | |||
| 25 | 26 | 27 | |||
| 1860 Feb 07 | 1878 Feb 17 | 1896 Feb 28 | |||
| 28 | 29 | 30 | |||
| 1914 Mar 12 | 1932 Mar 22 | 1950 Apr 02 | |||
 |  |  |  | |  |
| 31 | 32 | 33 | |||
| 1968 Apr 13 | 1986 Apr 24 | 2004 May 04 | |||
 |  |  |  |  |  |
| 34 | 35 | 36 | |||
| 2022 May 16 | 2040 May 26 | 2058 Jun 06 | |||
|  |  |  |  |  |
| 37 | 38 | 39 | |||
| 2076 Jun 17 | 2094 Jun 28 | 2112 Jul 09 | |||
 |  | | | ||
| 40 | 41 | 42 | |||
| 2130 Jul 21 | 2148 Jul 31 | 2166 Aug 11 | |||
| 43 | |||||
| 2184 Aug 21 | |||||
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 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1810 Sep 13 (Saros 105) | 1821 Aug 13 (Saros 106) | 1832 Jul 12 (Saros 107) | 1843 Jun 12 (Saros 108) | 1854 May 12 (Saros 109) | |||||
| 1865 Apr 11 (Saros 110) | 1876 Mar 10 (Saros 111) | 1887 Feb 08 (Saros 112) | 1898 Jan 08 (Saros 113) | 1908 Dec 07 (Saros 114) | |||||
 |  | ||||||||
| 1919 Nov 07 (Saros 115) | 1930 Oct 07 (Saros 116) | 1941 Sep 05 (Saros 117) | 1952 Aug 05 (Saros 118) | 1963 Jul 06 (Saros 119) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1974 Jun 04 (Saros 120) | 1985 May 04 (Saros 121) | 1996 Apr 04 (Saros 122) | 2007 Mar 03 (Saros 123) | 2018 Jan 31 (Saros 124) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2028 Dec 31 (Saros 125) | 2039 Nov 30 (Saros 126) | 2050 Oct 30 (Saros 127) | 2061 Sep 29 (Saros 128) | 2072 Aug 28 (Saros 129) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2083 Jul 29 (Saros 130) | 2094 Jun 28 (Saros 131) | 2105 May 28 (Saros 132) | 2116 Apr 27 (Saros 133) | 2127 Mar 28 (Saros 134) | |||||
 |  | | | ||||||
| 2138 Feb 24 (Saros 135) | 2149 Jan 23 (Saros 136) | 2159 Dec 24 (Saros 137) | 2170 Nov 23 (Saros 138) | 2181 Oct 22 (Saros 139) | |||||
| 2192 Sep 21 (Saros 140) | |||||||||
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 | |||||
|---|---|---|---|---|---|
| 1805 Jan 15 (Saros 121) | 1833 Dec 26 (Saros 122) | 1862 Dec 06 (Saros 123) | |||
| 1891 Nov 16 (Saros 124) | 1920 Oct 27 (Saros 125) | 1949 Oct 07 (Saros 126) | |||
 |  |  |  | ||
| 1978 Sep 16 (Saros 127) | 2007 Aug 28 (Saros 128) | 2036 Aug 07 (Saros 129) | |||
 |  |  |  |  |  |
| 2065 Jul 17 (Saros 130) | 2094 Jun 28 (Saros 131) | 2123 Jun 09 (Saros 132) | |||
 |  | | |  | |
| 2152 May 18 (Saros 133) | 2181 Apr 29 (Saros 134) | ||||
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (ahalf saros).[9] This lunar eclipse is related to two annular solar eclipses ofSolar Saros 138.
| June 22, 2085 | July 4, 2103 |
|---|---|
 |  |
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