| Penumbral eclipse | |||||||||
 The Moon's hourly motion shown right to left | |||||||||
| Date | February 22, 2035 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | −1.0357 | ||||||||
| Magnitude | −0.0523 | ||||||||
| Saros cycle | 114 (60 of 71) | ||||||||
| Penumbral | 255 minutes, 42 seconds | ||||||||
| |||||||||
A penumbrallunar eclipse will occur at the Moon’sascending node of orbit on Thursday, February 22,2035,[1] with an umbralmagnitude of −0.0523. 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 4.3 days afterperigee (on February 18, 2035, at 0:40 UTC), the Moon's apparent diameter will be larger.[2]
The eclipse will be completely visible overnortheast Asia andNorth America, seen rising overeast Asia andAustralia and setting overSouth 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 | 0.96629 |
| Umbral Magnitude | −0.05232 |
| Gamma | −1.03672 |
| Sun Right Ascension | 22h21m54.2s |
| Sun Declination | -10°11'53.9" |
| Sun Semi-Diameter | 16'10.2" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 10h20m48.3s |
| Moon Declination | +09°13'43.5" |
| Moon Semi-Diameter | 15'52.5" |
| Moon Equatorial Horizontal Parallax | 0°58'15.8" |
| ΔT | 76.5 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.
| February 22 Ascending node (full moon) | March 9 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 17, 2038 andDecember 11, 2038 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 2035 to 2038 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 114 | 2035 Feb 22 | Penumbral | −1.0357 | 119 | 2035 Aug 19 | Partial | 0.9433 | |
| 124 | 2036 Feb 11 | Total | −0.3110 | 129 | 2036 Aug 07 | Total | 0.2004 | |
| 134 | 2037 Jan 31 | Total | 0.3619 | 139 | 2037 Jul 27 | Partial | −0.5582 | |
| 144 | 2038 Jan 21 | Penumbral | 1.0710 | 149 | 2038 Jul 16 | Penumbral | −1.2837 | |
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 1904 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1904 Mar 02 (Saros 102) | 1915 Jan 31 (Saros 103) | ||||||||
 |  |  |  | ||||||
| 1969 Aug 27 (Saros 108) | 1980 Jul 27 (Saros 109) | 1991 Jun 27 (Saros 110) | 2002 May 26 (Saros 111) | ||||||
 |  |  |  |  |  |  |  | ||
| 2013 Apr 25 (Saros 112) | 2024 Mar 25 (Saros 113) | 2035 Feb 22 (Saros 114) | 2046 Jan 22 (Saros 115) | 2056 Dec 22 (Saros 116) | |||||
 |  |  |  | | |  |  |  |  |
| 2067 Nov 21 (Saros 117) | 2078 Oct 21 (Saros 118) | 2089 Sep 19 (Saros 119) | 2100 Aug 19 (Saros 120) | 2111 Jul 21 (Saros 121) | |||||
 |  | ||||||||
| 2122 Jun 20 (Saros 122) | 2133 May 19 (Saros 123) | 2144 Apr 18 (Saros 124) | 2155 Mar 19 (Saros 125) | 2166 Feb 15 (Saros 126) | |||||
| 2177 Jan 14 (Saros 127) | 2187 Dec 15 (Saros 128) | 2198 Nov 13 (Saros 129) | |||||||
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 | |||||
|---|---|---|---|---|---|
| 1803 Aug 03 (Saros 106) | 1832 Jul 12 (Saros 107) | 1861 Jun 22 (Saros 108) | |||
| 1890 Jun 03 (Saros 109) | 1919 May 15 (Saros 110) | 1948 Apr 23 (Saros 111) | |||
 |  |  |  | ||
| 1977 Apr 04 (Saros 112) | 2006 Mar 14 (Saros 113) | 2035 Feb 22 (Saros 114) | |||
 |  |  |  | | |
| 2064 Feb 02 (Saros 115) | 2093 Jan 12 (Saros 116) | 2121 Dec 24 (Saros 117) | |||
| 2150 Dec 04 (Saros 118) | 2179 Nov 14 (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 17, 2026 | February 28, 2044 |
|---|---|
 |  |
_(cropped).jpg)
