| Total eclipse | |||||||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||||||
| Date | February 9, 1990 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.4148 | ||||||||||||||||
| Magnitude | 1.0750 | ||||||||||||||||
| Saros cycle | 133 (25 of 71) | ||||||||||||||||
| Totality | 42 minutes, 19 seconds | ||||||||||||||||
| Partiality | 204 minutes, 17 seconds | ||||||||||||||||
| Penumbral | 339 minutes, 35 seconds | ||||||||||||||||
| |||||||||||||||||
A totallunar eclipse occurred at the Moon’sdescending node of orbit on Friday, February 9, 1990,[1] with an umbralmagnitude of 1.0750. 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. The Moon's apparent diameter will be near the average diameter because it will occur 7.7 days afterperigee (on February 2, 1990, at 2:40 UTC) and 6.75 days beforeapogee (on February 16, 1990, at 13:05 UTC).[2]
The eclipse was completely visible overeast Africa,eastern Europe, andAsia, seen rising over northeasternNorth America, easternSouth America,western Europe andwest andcentral Africa and setting overAustralia, northwestern North America, and the western and centralPacific 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 | 2.11912 |
| Umbral Magnitude | 1.07499 |
| Gamma | −0.41481 |
| Sun Right Ascension | 21h32m41.8s |
| Sun Declination | -14°34'08.6" |
| Sun Semi-Diameter | 16'12.6" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 09h32m01.7s |
| Moon Declination | +14°12'35.9" |
| Moon Semi-Diameter | 15'31.5" |
| Moon Equatorial Horizontal Parallax | 0°56'58.5" |
| ΔT | 56.9 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.
| January 26 Ascending node (new moon) | February 9 Descending node (full moon) |
|---|---|
 | |
| Annular solar eclipse Solar Saros 121 | Total lunar eclipse Lunar Saros 133 |
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 lunar eclipses onJune 27, 1991 (penumbral) andDecember 21, 1991 (partial) occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 1988 to 1991 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 113 | 1988 Mar 03 | Penumbral | 0.9886 | 118 | 1988 Aug 27 | Partial | −0.8682 | |
| 123 | 1989 Feb 20 | Total | 0.2935 | 128 | 1989 Aug 17 | Total | −0.1491 | |
| 133 | 1990 Feb 09 | Total | −0.4148 | 138 | 1990 Aug 06 | Partial | 0.6374 | |
| 143 | 1991 Jan 30 | Penumbral | −1.0752 | 148 | 1991 Jul 26 | Penumbral | 1.4370 | |
This eclipse is a part ofSaros series 133, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on May 13, 1557. It contains partial eclipses from August 7, 1683 through December 17, 1899; total eclipses fromDecember 28, 1917 through August 3, 2278; and a second set of partial eclipses from August 14, 2296 through March 11, 2639. The series ends at member 71 as a penumbral eclipse on June 29, 2819.
The longest duration of totality will be produced by member 35 at 101 minutes, 41 seconds onMay 30, 2170. All eclipses in this series occur at the Moon’sdescending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series will occur on2170 May 30, lasting 101 minutes, 41 seconds.[7] | Penumbral | Partial | Total | Central |
| 1557 May 13 | 1683 Aug 07 | 1917 Dec 28 | 2098 Apr 15 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2224 Jul 01 | 2278 Aug 03 | 2639 Mar 11 | 2819 Jun 29 | |
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 15–36 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 15 | 16 | 17 | |||
| 1809 Oct 23 | 1827 Nov 03 | 1845 Nov 14 | |||
| 18 | 19 | 20 | |||
| 1863 Nov 25 | 1881 Dec 05 | 1899 Dec 17 | |||
| 21 | 22 | 23 | |||
| 1917 Dec 28 | 1936 Jan 08 | 1954 Jan 19 | |||
|  |  |  |  |  |
| 24 | 25 | 26 | |||
| 1972 Jan 30 | 1990 Feb 09 | 2008 Feb 21 | |||
 |  | | |  |  |
| 27 | 28 | 29 | |||
| 2026 Mar 03 | 2044 Mar 13 | 2062 Mar 25 | |||
 |  |  |  | ||
| 30 | 31 | 32 | |||
| 2080 Apr 04 | 2098 Apr 15 | 2116 Apr 27 | |||
 |  | |  | ||
| 33 | 34 | 35 | |||
| 2134 May 08 | 2152 May 18 | 2170 May 30 | |||
| 36 | |||||
| 2188 Jun 09 | |||||
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 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1804 Jul 22 (Saros 116) | 1815 Jun 21 (Saros 117) | 1826 May 21 (Saros 118) | 1837 Apr 20 (Saros 119) | 1848 Mar 19 (Saros 120) | |||||
| 1859 Feb 17 (Saros 121) | 1870 Jan 17 (Saros 122) | 1880 Dec 16 (Saros 123) | 1891 Nov 16 (Saros 124) | 1902 Oct 17 (Saros 125) | |||||
 |  | ||||||||
| 1913 Sep 15 (Saros 126) | 1924 Aug 14 (Saros 127) | 1935 Jul 16 (Saros 128) | 1946 Jun 14 (Saros 129) | 1957 May 13 (Saros 130) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1968 Apr 13 (Saros 131) | 1979 Mar 13 (Saros 132) | 1990 Feb 09 (Saros 133) | 2001 Jan 09 (Saros 134) | 2011 Dec 10 (Saros 135) | |||||
 |  |  |  | | |  |  |  |  |
| 2022 Nov 08 (Saros 136) | 2033 Oct 08 (Saros 137) | 2044 Sep 07 (Saros 138) | 2055 Aug 07 (Saros 139) | 2066 Jul 07 (Saros 140) | |||||
 |  |  |  |  |  |  |  | ||
| 2077 Jun 06 (Saros 141) | 2088 May 05 (Saros 142) | 2099 Apr 05 (Saros 143) | 2110 Mar 06 (Saros 144) | 2121 Feb 02 (Saros 145) | |||||
 |  | ||||||||
| 2132 Jan 02 (Saros 146) | 2142 Dec 03 (Saros 147) | 2153 Nov 01 (Saros 148) | 2164 Sep 30 (Saros 149) | 2175 Aug 31 (Saros 150) | |||||
| 2186 Jul 31 (Saros 151) | 2197 Jun 29 (Saros 152) | ||||||||
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 | |||||
|---|---|---|---|---|---|
| 1816 Jun 10 (Saros 127) | 1845 May 21 (Saros 128) | 1874 May 01 (Saros 129) | |||
| 1903 Apr 12 (Saros 130) | 1932 Mar 22 (Saros 131) | 1961 Mar 02 (Saros 132) | |||
 |  |  |  |  |  |
| 1990 Feb 09 (Saros 133) | 2019 Jan 21 (Saros 134) | 2048 Jan 01 (Saros 135) | |||
| |  |  |  |  |
| 2076 Dec 10 (Saros 136) | 2105 Nov 21 (Saros 137) | 2134 Nov 02 (Saros 138) | |||
 |  | ||||
| 2163 Oct 12 (Saros 139) | 2192 Sep 21 (Saros 140) | ||||
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 annular solar eclipses ofSolar Saros 140.
| February 4, 1981 | February 16, 1999 |
|---|---|
 |  |
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