# September 1950 lunar eclipse

A total lunar eclipse occurred at the Moon’s ascending node of orbit on Tuesday, September 26, 1950, with an umbral magnitude of 1.0783. A lunar eclipse occurs when the Moon moves into the Earth'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 a solar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on the night 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's shadow is smaller. Occurring about 5.1 days before apogee (on October 1, 1950, at 5:30 UTC), the Moon's apparent diameter was smaller.
This lunar eclipse was the last of a tetrad, with four total lunar eclipses in series, the others being on April 13, 1949; October 7, 1949; and April 2, 1950.

## Visibility

The eclipse was completely visible over much of North and South America, seen rising over northwestern North America and the central Pacific Ocean and setting over Africa, Europe, and the Middle East.

## Eclipse details

Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.
September 26, 1950 Lunar Eclipse Parameters :
| Parameter | Value |
| Penumbral Magnitude | 2.13305 |
| Umbral Magnitude | 1.07834 |
| Gamma | 0.41012 |
| Sun Right Ascension | 12h09m13.2s |
| Sun Declination | -00°59'57.3" |
| Sun Semi-Diameter | 15'57.2" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 00h08m28.8s |
| Moon Declination | +01°19'50.3" |
| Moon Semi-Diameter | 15'07.6" |
| Moon Equatorial Horizontal Parallax | 0°55'30.9" |
| ΔT | 29.4 s |

## Eclipse season

This eclipse is part of an eclipse 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 a fortnight.
Eclipse season of September 1950 :
| September 12 Descending node (new moon) | September 26 Ascending node (full moon) |
| Total solar eclipse Solar Saros 124 | Total lunar eclipse Lunar Saros 136 |

## Related eclipses
### Eclipses in 1950

* An annular solar eclipse on March 18.
* A total lunar eclipse on April 2.
* A total solar eclipse on September 12.
* A total lunar eclipse on September 26.

### Metonic

* Preceded by: Lunar eclipse of December 8, 1946
* Followed by: Lunar eclipse of July 16, 1954

### Tzolkinex

* Preceded by: Lunar eclipse of August 15, 1943
* Followed by: Lunar eclipse of November 7, 1957

### Half-Saros

* Preceded by: Solar eclipse of September 21, 1941
* Followed by: Solar eclipse of October 2, 1959

### Tritos

* Preceded by: Lunar eclipse of October 28, 1939
* Followed by: Lunar eclipse of August 26, 1961

### Lunar Saros 136

* Preceded by: Lunar eclipse of September 14, 1932
* Followed by: Lunar eclipse of October 6, 1968

### Inex

* Preceded by: Lunar eclipse of October 16, 1921
* Followed by: Lunar eclipse of September 6, 1979

### Triad

* Preceded by: Lunar eclipse of November 25, 1863
* Followed by: Lunar eclipse of July 27, 2037

### Lunar eclipses of 1948–1951

This eclipse is a member of a semester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.
The penumbral lunar eclipses on February 21, 1951 and August 17, 1951 occur in the next lunar year eclipse set.
Lunar eclipse series sets from 1948 to 1951 :
| Descending node | Descending node | Descending node | Descending node | Ascending node | Ascending node | Ascending node | Ascending node |
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma |
| 111 | 1948 Apr 23 | Partial | 1.0017 | 116 | 1948 Oct 18 | Penumbral | −1.0245 |
| 121 | 1949 Apr 13 | Total | 0.2474 | 126 | 1949 Oct 07 | Total | −0.3219 |
| 131 | 1950 Apr 02 | Total | −0.4599 | 136 | 1950 Sep 26 | Total | 0.4101 |
| 141 | 1951 Mar 23 | Penumbral | −1.2099 | 146 | 1951 Sep 15 | Penumbral | 1.1187 |

### Saros 136

This eclipse is a part of Saros series 136, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on April 13, 1680. It contains partial eclipses from July 11, 1824 through September 14, 1932; total eclipses from September 26, 1950 through July 7, 2419; and a second set of partial eclipses from July 18, 2437 through October 3, 2563. The series ends at member 72 as a penumbral eclipse on June 1, 2960.
The longest duration of totality will be produced by member 35 at 101 minutes, 23 seconds on April 21, 2293. All eclipses in this series occur at the Moon’s ascending node of orbit.
| Greatest | First | First | First | First |
| The greatest eclipse of the series will occur on 2293 Apr 21, lasting 101 minutes, 23 seconds. | Penumbral | Partial | Total | Central |
| The greatest eclipse of the series will occur on 2293 Apr 21, lasting 101 minutes, 23 seconds. | 1680 Apr 13 | 1824 Jul 11 | 1950 Sep 26 | 2022 Nov 08 |
| Last ||||
| The greatest eclipse of the series will occur on 2293 Apr 21, lasting 101 minutes, 23 seconds. | Central | Total | Partial | Penumbral |
| The greatest eclipse of the series will occur on 2293 Apr 21, lasting 101 minutes, 23 seconds. | 2365 Jun 04 | 2419 Jul 07 | 2563 Oct 03 | 2960 Jun 01 |
Eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
Series members 8–29 occur between 1801 and 2200: :
| 8 | 8 | 9 | 9 | 10 | 10 |
| 1806 Jun 30 | 1806 Jun 30 | 1824 Jul 11 | 1824 Jul 11 | 1842 Jul 22 | 1842 Jul 22 |
| 11 | 11 | 12 | 12 | 13 | 13 |
| 1860 Aug 01 | 1860 Aug 01 | 1878 Aug 13 | 1878 Aug 13 | 1896 Aug 23 | 1896 Aug 23 |
| 14 | 14 | 15 | 15 | 16 | 16 |
| 1914 Sep 04 | 1914 Sep 04 | 1932 Sep 14 | 1932 Sep 14 | 1950 Sep 26 | 1950 Sep 26 |
| 17 | 17 | 18 | 18 | 19 | 19 |
| 1968 Oct 06 | 1968 Oct 06 | 1986 Oct 17 | 1986 Oct 17 | 2004 Oct 28 | 2004 Oct 28 |
| 20 | 20 | 21 | 21 | 22 | 22 |
| 2022 Nov 08 | 2022 Nov 08 | 2040 Nov 18 | 2040 Nov 18 | 2058 Nov 30 | 2058 Nov 30 |
| 23 | 23 | 24 | 24 | 25 | 25 |
| 2076 Dec 10 | 2076 Dec 10 | 2094 Dec 21 | 2094 Dec 21 | 2113 Jan 02 | 2113 Jan 02 |
| 26 | 26 | 27 | 27 | 28 | 28 |
| 2131 Jan 13 | 2131 Jan 13 | 2149 Jan 23 | 2149 Jan 23 | 2167 Feb 04 | 2167 Feb 04 |
| 29 ||
| 2185 Feb 14 ||

### Tritos series

This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic 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 :
| 1808 Nov 03 (Saros 123) | 1808 Nov 03 (Saros 123) | 1819 Oct 03 (Saros 124) | 1819 Oct 03 (Saros 124) | 1830 Sep 02 (Saros 125) | 1830 Sep 02 (Saros 125) | 1841 Aug 02 (Saros 126) | 1841 Aug 02 (Saros 126) | 1852 Jul 01 (Saros 127) | 1852 Jul 01 (Saros 127) |
| 1863 Jun 01 (Saros 128) | 1863 Jun 01 (Saros 128) | 1874 May 01 (Saros 129) | 1874 May 01 (Saros 129) | 1885 Mar 30 (Saros 130) | 1885 Mar 30 (Saros 130) | 1896 Feb 28 (Saros 131) | 1896 Feb 28 (Saros 131) | 1907 Jan 29 (Saros 132) | 1907 Jan 29 (Saros 132) |
| 1917 Dec 28 (Saros 133) | 1917 Dec 28 (Saros 133) | 1928 Nov 27 (Saros 134) | 1928 Nov 27 (Saros 134) | 1939 Oct 28 (Saros 135) | 1939 Oct 28 (Saros 135) | 1950 Sep 26 (Saros 136) | 1950 Sep 26 (Saros 136) | 1961 Aug 26 (Saros 137) | 1961 Aug 26 (Saros 137) |
| 1972 Jul 26 (Saros 138) | 1972 Jul 26 (Saros 138) | 1983 Jun 25 (Saros 139) | 1983 Jun 25 (Saros 139) | 1994 May 25 (Saros 140) | 1994 May 25 (Saros 140) | 2005 Apr 24 (Saros 141) | 2005 Apr 24 (Saros 141) | 2016 Mar 23 (Saros 142) | 2016 Mar 23 (Saros 142) |
| 2027 Feb 20 (Saros 143) | 2027 Feb 20 (Saros 143) | 2038 Jan 21 (Saros 144) | 2038 Jan 21 (Saros 144) | 2048 Dec 20 (Saros 145) | 2048 Dec 20 (Saros 145) | 2059 Nov 19 (Saros 146) | 2059 Nov 19 (Saros 146) | 2070 Oct 19 (Saros 147) | 2070 Oct 19 (Saros 147) |
| 2081 Sep 18 (Saros 148) | 2081 Sep 18 (Saros 148) | 2092 Aug 17 (Saros 149) | 2092 Aug 17 (Saros 149) | 2103 Jul 19 (Saros 150) | 2103 Jul 19 (Saros 150) | 2114 Jun 18 (Saros 151) | 2114 Jun 18 (Saros 151) | 2125 May 17 (Saros 152) | 2125 May 17 (Saros 152) |
| 2136 Apr 16 (Saros 153) | 2136 Apr 16 (Saros 153) | | | | | 2169 Jan 13 (Saros 156) | 2169 Jan 13 (Saros 156) | | |
| 2190 Nov 12 (Saros 158) ||

### Inex series

This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic 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 :
| 1806 Jan 05 (Saros 131) | 1806 Jan 05 (Saros 131) | 1834 Dec 16 (Saros 132) | 1834 Dec 16 (Saros 132) | 1863 Nov 25 (Saros 133) | 1863 Nov 25 (Saros 133) |
| 1892 Nov 04 (Saros 134) | 1892 Nov 04 (Saros 134) | 1921 Oct 16 (Saros 135) | 1921 Oct 16 (Saros 135) | 1950 Sep 26 (Saros 136) | 1950 Sep 26 (Saros 136) |
| 1979 Sep 06 (Saros 137) | 1979 Sep 06 (Saros 137) | 2008 Aug 16 (Saros 138) | 2008 Aug 16 (Saros 138) | 2037 Jul 27 (Saros 139) | 2037 Jul 27 (Saros 139) |
| 2066 Jul 07 (Saros 140) | 2066 Jul 07 (Saros 140) | 2095 Jun 17 (Saros 141) | 2095 Jun 17 (Saros 141) | 2124 May 28 (Saros 142) | 2124 May 28 (Saros 142) |
| 2153 May 08 (Saros 143) | 2153 May 08 (Saros 143) | 2182 Apr 18 (Saros 144) | 2182 Apr 18 (Saros 144) |

### Half-Saros cycle

A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros). This lunar eclipse is related to two total solar eclipses of Solar Saros 143.
| September 21, 1941 | October 2, 1959 |