| Partial eclipse | |||||||||||||
 Partiality as viewed fromBucharest, Romania, 18:37 UTC | |||||||||||||
| Date | September 7, 2006 | ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.9262 | ||||||||||||
| Magnitude | 0.1837 | ||||||||||||
| Saros cycle | 118 (51 of 74) | ||||||||||||
| Partiality | 91 minutes, 6 seconds | ||||||||||||
| Penumbral | 254 minutes, 23 seconds | ||||||||||||
| |||||||||||||
A partiallunar eclipse occurred at the Moon’sascending node of orbit on Thursday, September 7, 2006,[1] with an umbralmagnitude of 0.1837. A lunar eclipse occurs when theMoon moves into theEarth's shadow, causing the Moon to be darkened. A partial lunar eclipse occurs when one part of the Moon is in the Earth's umbra, while the other part is in 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 4 hours beforeperigee (on September 7, 2006, at 23:00 UTC), the Moon's apparent diameter was larger.[2]
The eclipse was completely visible overAsia,east Africa,eastern Europe and westernAustralia, seen rising overwest Africa andwestern Europe and setting over easternAustralia and the westernPacific Ocean.[3]
 |  Hourly motion shown right to left |  The Moon's hourly motion across the Earth's shadow in the constellation ofAquarius. |
 Visibility map | ||
Degania A, Israel
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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 | 1.13488 |
| Umbral Magnitude | 0.18568 |
| Gamma | −0.92619 |
| Sun Right Ascension | 11h04m47.1s |
| Sun Declination | +05°54'23.1" |
| Sun Semi-Diameter | 15'52.4" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 23h06m35.6s |
| Moon Declination | -06°44'25.6" |
| Moon Semi-Diameter | 16'43.3" |
| Moon Equatorial Horizontal Parallax | 1°01'22.3" |
| ΔT | 65.1 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.
| September 7 Ascending node (full moon) | September 22 Descending node (new moon) |
|---|---|
|  |
| Partial lunar eclipse Lunar Saros 118 | Annular solar eclipse Solar Saros 144 |
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 onJuly 7, 2009 (penumbral) andDecember 31, 2009 (partial) occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 2006 to 2009 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
113.jpg) | 2006 Mar 14 | Penumbral | 1.0211 | 118 | 2006 Sep 7 | Partial | −0.9262 | |
123 | 2007 Mar 03 | Total | 0.3175 | 128 | 2007 Aug 28 | Total | −0.2146 | |
133 | 2008 Feb 21 | Total | −0.3992 | 138 | 2008 Aug 16 | Partial | 0.5646 | |
143 | 2009 Feb 09 | Penumbral | −1.0640 | 148 | 2009 Aug 06 | Penumbral | 1.3572 | |
TheMetonic cycle repeats nearly exactly every 19 years and represents aSaros cycle plus one lunar year. Because it occurs on the same calendar date, the Earth's shadow will in nearly the same location relative to the background stars.
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This eclipse is a part ofSaros series 118, repeating every 18 years, 11 days, and containing 73 events. The series started with a penumbral lunar eclipse on March 2, 1105. It contains partial eclipses from June 8, 1267 through August 12, 1375; total eclipses from August 22, 1393 through June 22, 1880; and a second set of partial eclipses from July 3, 1898 throughSeptember 18, 2024. The series ends at member 73 as a penumbral eclipse on May 7, 2403.
The longest duration of totality was produced by member 37 at 99 minutes, 22 seconds on April 7, 1754. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1754 Apr 07, lasting 99 minutes, 22 seconds.[7] | Penumbral | Partial | Total | Central |
| 1105 Mar 02 | 1267 Jun 08 | 1393 Aug 22 | 1465 Oct 04 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1826 May 21 | 1880 Jun 22 | 2024 Sep 18 | 2403 May 07 | |
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 40–61 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 40 | 41 | 42 | |||
| 1808 May 10 | 1826 May 21 | 1844 May 31 | |||
| 43 | 44 | 45 | |||
| 1862 Jun 12 | 1880 Jun 22 | 1898 Jul 03 | |||
| 46 | 47 | 48 | |||
| 1916 Jul 15 | 1934 Jul 26 | 1952 Aug 05 | |||
 |  |  |  |  |  |
| 49 | 50 | 51 | |||
| 1970 Aug 17 | 1988 Aug 27 | 2006 Sep 07 | |||
 |  |  |  | | |
| 52 | 53 | 54 | |||
| 2024 Sep 18 | 2042 Sep 29 | 2060 Oct 09 | |||
|  |  |  | ||
| 55 | 56 | 57 | |||
| 2078 Oct 21 | 2096 Oct 31 | 2114 Nov 12 | |||
| 58 | 59 | 60 | |||
| 2132 Nov 23 | 2150 Dec 04 | 2168 Dec 14 | |||
| 61 | |||||
| 2186 Dec 26 | |||||
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 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1810 Mar 21 (Saros 100) | 1821 Feb 17 (Saros 101) | 1832 Jan 17 (Saros 102) | 1842 Dec 17 (Saros 103) | ||||||
| 1864 Oct 15 (Saros 105) | 1875 Sep 15 (Saros 106) | 1886 Aug 14 (Saros 107) | 1897 Jul 14 (Saros 108) | 1908 Jun 14 (Saros 109) | |||||
 |  | ||||||||
| 1919 May 15 (Saros 110) | 1930 Apr 13 (Saros 111) | 1941 Mar 13 (Saros 112) | 1952 Feb 11 (Saros 113) | 1963 Jan 09 (Saros 114) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1973 Dec 10 (Saros 115) | 1984 Nov 08 (Saros 116) | 1995 Oct 08 (Saros 117) | 2006 Sep 07 (Saros 118) | 2017 Aug 07 (Saros 119) | |||||
 |  |  |  |  |  | | |  |  |
| 2028 Jul 06 (Saros 120) | 2039 Jun 06 (Saros 121) | 2050 May 06 (Saros 122) | 2061 Apr 04 (Saros 123) | 2072 Mar 04 (Saros 124) | |||||
 |  |  |  |  |  | ||||
| 2083 Feb 02 (Saros 125) | 2094 Jan 01 (Saros 126) | 2104 Dec 02 (Saros 127) | 2115 Nov 02 (Saros 128) | 2126 Oct 01 (Saros 129) | |||||
| 2137 Aug 30 (Saros 130) | 2148 Jul 31 (Saros 131) | 2159 Jun 30 (Saros 132) | 2170 May 30 (Saros 133) | 2181 Apr 29 (Saros 134) | |||||
| 2192 Mar 28 (Saros 135) | |||||||||
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 | |||||
|---|---|---|---|---|---|
| 1804 Jan 26 (Saros 111) | 1833 Jan 06 (Saros 112) | 1861 Dec 17 (Saros 113) | |||
| 1890 Nov 26 (Saros 114) | 1919 Nov 07 (Saros 115) | 1948 Oct 18 (Saros 116) | |||
 |  |  |  | ||
| 1977 Sep 27 (Saros 117) | 2006 Sep 07 (Saros 118) | 2035 Aug 19 (Saros 119) | |||
 |  | | |  |  |
| 2064 Jul 28 (Saros 120) | 2093 Jul 08 (Saros 121) | 2122 Jun 20 (Saros 122) | |||
| 2151 May 30 (Saros 123) | 2180 May 09 (Saros 124) | ||||
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 125.
| September 2, 1997 | September 13, 2015 |
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