| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | June 15, 2049 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | 1.4068 | ||||||||
| Magnitude | −0.6970 | ||||||||
| Saros cycle | 150 (3 of 71) | ||||||||
| Penumbral | 131 minutes, 58 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sascending node of orbit on Tuesday, June 15, 2049,[1] with an umbralmagnitude of −0.6970. 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 only about 23.5 hours beforeperigee (on June 16, 2049, at 18:40 UTC), the Moon's apparent diameter will be larger.[2]
The eclipse will be completely visible overcentral andeast Africa,eastern Europe, much ofAsia,Australia, andAntarctica, seen rising overwest Africa andwestern Europe and setting overnortheast Asia and the westernPacific Ocean.[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 | 0.25260 |
| Umbral Magnitude | −0.69700 |
| Gamma | 1.40692 |
| Sun Right Ascension | 05h38m45.5s |
| Sun Declination | +23°20'31.0" |
| Sun Semi-Diameter | 15'44.8" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 17h38m24.2s |
| Moon Declination | -21°55'02.3" |
| Moon Semi-Diameter | 16'34.9" |
| Moon Equatorial Horizontal Parallax | 1°00'51.4" |
| ΔT | 84.8 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.
| May 17 Ascending node (full moon) | May 31 Descending node (new moon) | June 15 Ascending node (full moon) |
|---|---|---|
 |  | |
| Penumbral lunar eclipse Lunar Saros 112 | Annular solar eclipse Solar Saros 138 | Penumbral lunar eclipse Lunar Saros 150 |
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 eclipses onMay 17, 2049 andNovember 9, 2049 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 2046 to 2049 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 115 | 2046 Jan 22 | Partial | 0.9885 | 120 | 2046 Jul 18 | Partial | −0.8691 | |
| 125 | 2047 Jan 12 | Total | 0.3317 | 130 | 2047 Jul 07 | Total | −0.0636 | |
| 135 | 2048 Jan 01 | Total | −0.3745 | 140 | 2048 Jun 26 | Partial | 0.6796 | |
| 145 | 2048 Dec 20 | Penumbral | −1.0624 | 150 | 2049 Jun 15 | Penumbral | 1.4068 | |
This eclipse is a part ofSaros series 150, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse onMay 25, 2013. It contains partial eclipses from August 20, 2157 through April 19, 2554; total eclipses from April 29, 2572 through August 28, 2770; and a second set of partial eclipses from September 7, 2788 through February 8, 3041. The series ends at member 71 as a penumbral eclipse on June 30, 3275.
The longest duration of totality will be produced by member 36 at 105 minutes, 16 seconds on July 4, 2680. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series will occur on2680 Jul 04, lasting 105 minutes, 16 seconds.[7] | Penumbral | Partial | Total | Central |
2013 May 25 | 2157 Aug 20 | 2572 Apr 29 | 2626 Jun 02 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2734 Aug 07 | 2770 Aug 28 | 3041 Feb 08 | 3275 Jun 30 | |
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 1–11 occur between 2013 and 2200: | |||||
|---|---|---|---|---|---|
| 1 | 2 | 3 | |||
| 2013 May 25 | 2031 Jun 05 | 2049 Jun 15 | |||
|  |  |  | | |
| 4 | 5 | 6 | |||
| 2067 Jun 27 | 2085 Jul 07 | 2103 Jul 19 | |||
| 7 | 8 | 9 | |||
| 2121 Jul 30 | 2139 Aug 10 | 2157 Aug 20 | |||
| 10 | 11 | ||||
| 2175 Aug 31 | 2193 Sep 11 | ||||
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 2147 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1809 Apr 30 (Saros 128) | 1820 Mar 29 (Saros 129) | 1831 Feb 26 (Saros 130) | 1842 Jan 26 (Saros 131) | 1852 Dec 26 (Saros 132) | |||||
| 1863 Nov 25 (Saros 133) | 1874 Oct 25 (Saros 134) | 1885 Sep 24 (Saros 135) | 1896 Aug 23 (Saros 136) | 1907 Jul 25 (Saros 137) | |||||
 |  | ||||||||
| 1918 Jun 24 (Saros 138) | 1929 May 23 (Saros 139) | 1940 Apr 22 (Saros 140) | 1951 Mar 23 (Saros 141) | 1962 Feb 19 (Saros 142) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1973 Jan 18 (Saros 143) | 1983 Dec 20 (Saros 144) | 1994 Nov 18 (Saros 145) | 2005 Oct 17 (Saros 146) | 2016 Sep 16 (Saros 147) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2027 Aug 17 (Saros 148) | 2038 Jul 16 (Saros 149) | 2049 Jun 15 (Saros 150) | |||||||
 |  |  |  | | | ||||
| 2114 Dec 12 (Saros 156) | |||||||||
| 2147 Sep 09 (Saros 159) | |||||||||
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 | |||||
|---|---|---|---|---|---|
| 1817 Nov 23 (Saros 142) | 1846 Nov 03 (Saros 143) | 1875 Oct 14 (Saros 144) | |||
| 1904 Sep 24 (Saros 145) | 1933 Sep 04 (Saros 146) | 1962 Aug 15 (Saros 147) | |||
 |  |  |  |  |  |
| 1991 Jul 26 (Saros 148) | 2020 Jul 05 (Saros 149) | 2049 Jun 15 (Saros 150) | |||
 |  |  |  | | |
| 2107 May 07 (Saros 152) | 2136 Apr 16 (Saros 153) | ||||
| 2194 Mar 07 (Saros 155) | |||||
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 one partial solar eclipse ofSolar Saros 157.
| June 21, 2058 |
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