| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | March 4, 2053 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | −1.0530 | ||||||||
| Magnitude | −0.0796 | ||||||||
| Saros cycle | 114 (61 of 71) | ||||||||
| Penumbral | 251 minutes, 5 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sascending node of orbit on Tuesday, March 4, 2053,[1] with an umbralmagnitude of −0.0796. 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 4.1 days afterperigee (on February 28, 2053, at 15:30 UTC), the Moon's apparent diameter will be larger.[2]
The eclipse will be completely visible overAsia andAustralia, seen rising overAfrica andEurope and setting over northwesternNorth America and the centralPacific Ocean.[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 | 0.93338 |
| Umbral Magnitude | −0.07963 |
| Gamma | −1.05310 |
| Sun Right Ascension | 23h03m14.8s |
| Sun Declination | -06°03'47.9" |
| Sun Semi-Diameter | 16'07.7" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 11h02m02.1s |
| Moon Declination | +05°04'58.9" |
| Moon Semi-Diameter | 15'55.3" |
| Moon Equatorial Horizontal Parallax | 0°58'26.0" |
| ΔT | 87.2 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.
| March 4 Ascending node (full moon) | March 20 Descending node (new moon) |
|---|---|
|  |
| Penumbral lunar eclipse Lunar Saros 114 | Annular solar eclipse Solar Saros 140 |
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 onJune 27, 2056 andDecember 22, 2056 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 2053 to 2056 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 114 | 2053 Mar 04 | Penumbral | −1.0530 | 119 | 2053 Aug 29 | Penumbral | 1.0165 | |
| 124 | 2054 Feb 22 | Total | −0.3242 | 129 | 2054 Aug 18 | Total | 0.2806 | |
| 134 | 2055 Feb 11 | Total | 0.3526 | 139 | 2055 Aug 07 | Partial | −0.4769 | |
| 144 | 2056 Feb 01 | Penumbral | 1.0682 | 149 | 2056 Jul 26 | Partial | −1.2048 | |
This eclipse is a part ofSaros series 114, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on May 13, 971 AD. It contains partial eclipses from August 7, 1115 through February 18, 1440; total eclipses from February 28, 1458 through July 17, 1674; and a second set of partial eclipses from July 28, 1692 through November 26, 1890. The series ends at member 71 as a penumbral eclipse on June 22, 2233.
The longest duration of totality was produced by member 35 at 106 minutes, 5 seconds on May 24, 1584. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1584 May 24, lasting 106 minutes, 5 seconds.[7] | Penumbral | Partial | Total | Central |
| 971 May 13 | 1115 Aug 07 | 1458 Feb 28 | 1530 Apr 12 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1638 Jun 26 | 1674 Jul 17 | 1890 Nov 26 | 2233 Jun 22 | |
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 48–69 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 48 | 49 | 50 | |||
| 1818 Oct 14 | 1836 Oct 24 | 1854 Nov 04 | |||
| 51 | 52 | 53 | |||
| 1872 Nov 15 | 1890 Nov 26 | 1908 Dec 07 | |||
 |  | ||||
| 54 | 55 | 56 | |||
| 1926 Dec 19 | 1944 Dec 29 | 1963 Jan 09 | |||
 |  |  |  |  |  |
| 57 | 58 | 59 | |||
| 1981 Jan 20 | 1999 Jan 31 | 2017 Feb 11 | |||
 |  |  |  |  |  |
| 60 | 61 | 62 | |||
| 2035 Feb 22 | 2053 Mar 04 | 2071 Mar 16 | |||
 |  | | | ||
| 63 | 64 | 65 | |||
| 2089 Mar 26 | 2107 Apr 07 | 2125 Apr 18 | |||
| 66 | 67 | 68 | |||
| 2143 Apr 29 | 2161 May 09 | 2179 May 21 | |||
| 69 | |||||
| 2197 May 31 | |||||
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 1922 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1922 Mar 13 (Saros 102) | 1933 Feb 10 (Saros 103) | ||||||||
 |  |  |  | ||||||
| 1998 Aug 08 (Saros 109) | 2009 Jul 07 (Saros 110) | 2020 Jun 05 (Saros 111) | |||||||
 |  |  |  |  |  | ||||
| 2031 May 07 (Saros 112) | 2042 Apr 05 (Saros 113) | 2053 Mar 04 (Saros 114) | 2064 Feb 02 (Saros 115) | 2075 Jan 02 (Saros 116) | |||||
 |  |  |  | | | ||||
| 2085 Dec 01 (Saros 117) | 2096 Oct 31 (Saros 118) | 2107 Oct 02 (Saros 119) | 2118 Aug 31 (Saros 120) | 2129 Jul 31 (Saros 121) | |||||
| 2140 Jun 30 (Saros 122) | 2151 May 30 (Saros 123) | 2162 Apr 29 (Saros 124) | 2173 Mar 29 (Saros 125) | 2184 Feb 26 (Saros 126) | |||||
| 2195 Jan 26 (Saros 127) | |||||||||
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 | |||||
|---|---|---|---|---|---|
| 1821 Aug 13 (Saros 106) | 1850 Jul 24 (Saros 107) | 1879 Jul 03 (Saros 108) | |||
| 1908 Jun 14 (Saros 109) | 1937 May 25 (Saros 110) | 1966 May 04 (Saros 111) | |||
 |  |  |  |  |  |
| 1995 Apr 15 (Saros 112) | 2024 Mar 25 (Saros 113) | 2053 Mar 04 (Saros 114) | |||
 |  |  |  | | |
| 2082 Feb 13 (Saros 115) | 2111 Jan 25 (Saros 116) | 2140 Jan 04 (Saros 117) | |||
| 2168 Dec 14 (Saros 118) | 2197 Nov 24 (Saros 119) | ||||
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 total solar eclipses ofSolar Saros 121.
| February 28, 2044 | March 11, 2062 |
|---|---|
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