| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | May 17, 2049 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | −1.1337 | ||||||||
| Magnitude | −0.2073 | ||||||||
| Saros cycle | 112 (67 of 72) | ||||||||
| Penumbral | 224 minutes, 16 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sascending node of orbit on Monday, May 17, 2049,[1] with an umbralmagnitude of −0.2073. 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 1.9 days beforeperigee (on May 19, 2049, at 15:25 UTC), the Moon's apparent diameter will be larger.[2]
The eclipse will be completely visible overAustralia,Antarctica, and thePacific Ocean, seen rising overeast Asia and setting over much ofNorth andSouth America.[3]
 |
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 | 0.76505 |
| Umbral Magnitude | −0.20727 |
| Gamma | −1.13375 |
| Sun Right Ascension | 03h38m51.9s |
| Sun Declination | +19°28'58.4" |
| Sun Semi-Diameter | 15'49.0" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 15h38m12.8s |
| Moon Declination | -20°36'01.8" |
| Moon Semi-Diameter | 16'16.0" |
| Moon Equatorial Horizontal Parallax | 0°59'41.9" |
| ΔT | 84.7 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 eclipse onJune 15, 2049 occurs in the previous lunar year eclipse set.
| Lunar eclipse series sets from 2049 to 2052 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 112 | 2049 May 17 | Penumbral | −1.1337 | 117 | 2049 Nov 09 | Penumbral | 1.1964 | |
| 122 | 2050 May 06 | Total | −0.4181 | 127 | 2050 Oct 30 | Total | 0.4435 | |
| 132 | 2051 Apr 26 | Total | 0.3371 | 137 | 2051 Oct 19 | Total | −0.2542 | |
| 142 | 2052 Apr 14 | Penumbral | 1.0628 | 147 | 2052 Oct 08 | Partial | −0.9726 | |
This eclipse is a part ofSaros series 112, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on May 20, 859 AD. It contains partial eclipses from August 3, 985 AD through March 8, 1346; total eclipses from March 18, 1364 through August 27, 1616; and a second set of partial eclipses from September 7, 1634 throughApril 25, 2013. The series ends at member 72 as a penumbral eclipse onJuly 12, 2139.
The longest duration of totality was produced by member 36 at 99 minutes, 51 seconds on June 2, 1490. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1490 Jun 02, lasting 99 minutes, 51 seconds.[7] | Penumbral | Partial | Total | Central |
| 859 May 20 | 985 Aug 03 | 1364 Mar 18 | 1436 Apr 30 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1562 Jul 16 | 1616 Aug 27 | 2013 Apr 25 | 2139 Jul 12 | |
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 54–72 occur between 1801 and 2139: | |||||
|---|---|---|---|---|---|
| 54 | 55 | 56 | |||
| 1814 Dec 26 | 1833 Jan 06 | 1851 Jan 17 | |||
| 57 | 58 | 59 | |||
| 1869 Jan 28 | 1887 Feb 08 | 1905 Feb 19 | |||
 |  | ||||
| 60 | 61 | 62 | |||
| 1923 Mar 03 | 1941 Mar 13 | 1959 Mar 24 | |||
 |  |  |  |  |  |
| 63 | 64 | 65 | |||
| 1977 Apr 04 | 1995 Apr 15 | 2013 Apr 25 | |||
 |  |  |  | |  |
| 66 | 67 | 68 | |||
| 2031 May 07 | 2049 May 17 | 2067 May 28 | |||
 |  | | |  |  |
| 69 | 70 | 71 | |||
| 2085 Jun 08 | 2103 Jun 20 | 2121 Jun 30 | |||
| 72 | |||||
| 2139 Jul 12 | |||||
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 1940 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1940 Mar 23 (Saros 102) | 1951 Feb 21 (Saros 103) | ||||||||
 |  |  |  | ||||||
| 2027 Jul 18 (Saros 110) | 2038 Jun 17 (Saros 111) | ||||||||
 |  |  |  | ||||||
| 2049 May 17 (Saros 112) | 2060 Apr 15 (Saros 113) | 2071 Mar 16 (Saros 114) | 2082 Feb 13 (Saros 115) | 2093 Jan 12 (Saros 116) | |||||
| | ||||||||
| 2103 Dec 13 (Saros 117) | 2114 Nov 12 (Saros 118) | 2125 Oct 12 (Saros 119) | 2136 Sep 10 (Saros 120) | 2147 Aug 11 (Saros 121) | |||||
| 2158 Jul 11 (Saros 122) | 2169 Jun 09 (Saros 123) | 2180 May 09 (Saros 124) | 2191 Apr 09 (Saros 125) | ||||||
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 1846 and 2200 | |||||
|---|---|---|---|---|---|
| 1846 Oct 04 (Saros 105) | 1875 Sep 15 (Saros 106) | ||||
| 1933 Aug 05 (Saros 108) | 1962 Jul 17 (Saros 109) | 1991 Jun 27 (Saros 110) | |||
 |  |  |  |  |  |
| 2020 Jun 05 (Saros 111) | 2049 May 17 (Saros 112) | 2078 Apr 27 (Saros 113) | |||
 |  | | | ||
| 2107 Apr 07 (Saros 114) | 2136 Mar 18 (Saros 115) | 2165 Feb 26 (Saros 116) | |||
| 2194 Feb 05 (Saros 117) | |||||
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 119.
| May 11, 2040 | May 22, 2058 |
|---|---|
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