Visibility
| Partial eclipse | |||||||||||||
| Date | 17 August 1970 | ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.80534 | ||||||||||||
| Magnitude | 0.40797 | ||||||||||||
| Saros cycle | 118 (49 of 74) | ||||||||||||
| Partiality | 131 minutes, 22.5 seconds | ||||||||||||
| Penumbral | 270 minutes, 41.5 seconds | ||||||||||||
| |||||||||||||
A partial lunar eclipse took place on Monday, August 17, 1970, the second of two lunar eclipses in 1970, the first was on February 21 of that year. The Earth's shadow on the Moon was clearly visible in this eclipse, with 41% of the Moon in shadow; the partial eclipse lasted for 2 hours and 11 minutes. It was the second of two lunar eclipses in 1970. [1]
Penumbral Magnitude: 1.35215
Umbral Magnitude: 0.40797
Gamma: -0.80534
Date: Monday, 17 August 1970
Saros Series: 118th (49 of 73)
Greatest Eclipse: 1970 August 17 at 03:23:25.6 UTC
Sun Right Ascension: 9.74
Sun Declination: 13.6
Sun Diameter: 1895.8 arc-seconds
Moon Right Ascension: 21.77
Moon Declination: -14.3
Moon Diameter: 2007.8 arc-seconds
The total duration of the eclipse was 4 hours, 31 minutes.
The duration of the partial eclipse was 2 hours, 11 minutes.
| Lunar eclipse series sets from 1969–1973 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 108 | 1969 Aug 27  | Penumbral | −1.54066 | 113 | 1970 Feb 21  | Partial | 0.96198 | |
| 118 | 1970 Aug 17  | Partial | −0.80534 | 123 | 1971 Feb 10  | Total | 0.27413 | |
| 128 | 1971 Aug 6  | Total | −0.07944 | 133 | 1972 Jan 30  | Total | −0.42729 | |
| 138 | 1972 Jul 26  | Partial | 0.71167 | 143 | 1973 Jan 18  | Penumbral | −1.08446 | |
| 148 | 1973 Jul 15  | Penumbral | 1.51782 | |||||
| Last set | 1969 Sep 25 | Last set | 1969 Apr 2 | |||||
| Next set | 1973 Jun 15 | Next set | 1973 Dec 10 | |||||
This is the third of five Metonic lunar eclipses.
The Metonic cycle repeats nearly exactly every 19 years and represents a Saros 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.
| Descending node | Ascending node | |||||
|---|---|---|---|---|---|---|
| Saros | Date | Type | Saros | Date | Type | |
| 103 | 1951 Feb 21.88 | Penumbral | 108 | 1951 Aug 17.13 | Penumbral | |
 |  | |||||
| 113 | 1970 Feb 21.35 | Partial | 118 | 1970 Aug 17.14 | Partial | |
 |  | |||||
| 123 | 1989 Feb 20.64 | Total | 128 | 1989 Aug 17.13 | Total | |
 |  | |||||
| 133 | 2008 Feb 21.14 | Total | 138 | 2008 Aug 16.88 | Partial | |
 |  | |||||
| 143 | 2027 Feb 20.96 | Penumbral | 148 | 2027 Aug 17.30 | Penumbral | |
 |  | |||||
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros). [2] This lunar eclipse is related to two annular solar eclipses of Solar Saros 125.
| August 11, 1961 | August 22, 1979 |
|---|---|
 |  |
 | This lunar eclipse-related article is a stub. You can help Wikipedia by expanding it. |
A total lunar eclipse took place on 3 March 2007, the first of two eclipses in 2007. The moon entered the penumbral shadow at 20:18 UTC, and the umbral shadow at 21:30 UTC. The total phase lasted between 22:44 UTC and 23:58 UTC with a distinctive brick-red shade. The moon left the umbra shadow at 01:11 UTC and left the penumbra shadow at 02:24 UTC 2007-03-04. The second lunar eclipse of 2007 occurred on 28 August.
A total lunar eclipse occurred on February 20 and February 21, 2008. It was visible in the eastern evening sky on February 20 for all of North and South America, and on February 21 in the predawn western sky from most of Africa and Europe. Greatest Eclipse occurring on Thursday, February 21, 2008, at 03:26:03 UTC, totality lasting 49 minutes and 45.6 seconds.
A total solar eclipse occurred at the Moon's descending node of the orbit on August 1, 2008. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. It had a magnitude of 1.0394 that was visible from a narrow corridor through northern Canada (Nunavut), Greenland, central Russia, eastern Kazakhstan, western Mongolia and China. Occurring north of the arctic circle, it belonged to the so-called midnight sun eclipses. The largest city in the path of the eclipse was Novosibirsk in Russia. Occurring only 2.5 days after perigee, the Moon's apparent diameter was larger than average.
A total lunar eclipse will take place between Monday and Tuesday, June 25-26, 2029. A central total eclipse lasting 1 hour and 41 minutes 53 seconds will plunge the full Moon into deep darkness, as it passes right through the centre of the Earth's umbral shadow. While the visual effect of a total eclipse is variable, the Moon may be stained a deep orange or red color at maximum eclipse. It will be able to be seen from most of the Americas, Western Europe and Africa. The partial eclipse will last for 3 hours and 39 minutes 32 seconds in total.
A total lunar eclipse took place on Friday, October 17, 1986, the second of two total lunar eclipses in 1986, the first being on April 24, 1986. The Moon was plunged into darkness for 1 hour, 13 minutes and 41 seconds, in a deep total eclipse which saw the Moon 24.545% of its diameter inside the Earth's umbral shadow. The visual effect of this depends on the state of the Earth's atmosphere, but the Moon may have been stained a deep red colour. The partial eclipse lasted for 3 hours, 36 minutes and 49.5 seconds in total. The Moon was 5.4 days before apogee, making it 3.3% smaller than average.
A penumbral lunar eclipse took place on Tuesday, January 20, 1981, the first of two lunar eclipses in 1981. In a rare total penumbral eclipse, the entire Moon was partially shaded by the Earth, and the shading across the Moon should have been quite visible at maximum eclipse. The penumbral phase lasted for 4 hours and 24 minutes in all, though for most of it, the eclipse was extremely difficult or impossible to see. The moon's apparent diameter was larger because the eclipse occurred 5.2 days after perigee.
A total lunar eclipse took place on Saturday, April 13, 1968, the first of two total eclipses in 1968, the second being on October 6, 1968.
A partial lunar eclipse took place on Saturday, February 21, 1970. It was the first of two partial lunar eclipses in 1970, the other being on August 17 of the same year. A tiny bite out of the Moon may have been visible at maximum, though just 5% of the Moon was shadowed in a partial eclipse which lasted for 52 minutes and 42 seconds. A shading across the moon from the Earth's penumbral shadow should have been visible at maximum eclipse.
A total lunar eclipse took place on Monday, April 24, 1967, the first of two total lunar eclipses in 1967, the second being on October 18, 1967.
An annular solar eclipse occurred at the Moon's ascending node of the orbit on January 15, 2010, with a magnitude of 0.91903. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. It was the longest annular solar eclipse of the millennium, and the longest until December 23, 3043, with the length of maximum eclipse of 11 minutes, 7.8 seconds, and the longest duration of 11 minutes, 10.7 seconds. This is about 4 minutes longer than total solar eclipses could ever get.
A total solar eclipse took place on 13–14 November 2012 (UTC). Because it crossed the International Date Line it began in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. Its greatest magnitude was 1.0500, occurring only 12 hours before perigee, with greatest eclipse totality lasting just over four minutes. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide.
An annular solar eclipse took place on February 26, 2017. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring only 4.7 days before perigee, the Moon's apparent diameter was larger. The moon's apparent diameter was just over 0.7% smaller than the Sun's.
An annular solar eclipse occurred on December 14, 1955. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
An annular solar eclipse occurred at the Moon's descending node of the orbit on February 4–5, 1981. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. This annular solar eclipse was large because the Moon covered 99.4% of the Sun, with a path width of only 25 km . It was visible in Australia, crossing over Tasmania and southern Stewart Island of New Zealand near sunrise on February 5 (Thursday), and ended at sunset over western South America on February 4 (Wednesday). Occurring only 4 days before perigee, the moon's apparent diameter was larger.
A total solar eclipse occurred on July 20, 1963. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is at least the same size as the Sun's or larger, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with a partial solar eclipse visible over the surrounding region thousands of kilometres wide. Totality was visible from Hokkaido in Japan and Kuril Islands in Soviet Union on July 21, and Alaska, and Maine in the United States and also Canada on July 20. Astronomer Charles H. Smiley observed the eclipse from a U.S. Air Force F-104D Starfighter supersonic aircraft that was "racing the moon's shadow" at 1,300 mph (2,100 km/h) extending the duration of totality to 4 minutes 3 seconds. The moon was 375,819 km from the Earth.
A total solar eclipse occurred on June 8–9, 1956. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. It began near sunrise over New Zealand on June 9 (Saturday), and ended west of South America on June 8 (Friday).
An annular solar eclipse will occur on Monday, November 15, 2077, with a magnitude of 0.9371. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partially obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. The path of annularity will cross North America and South America. This will be the 47th solar eclipse of Saros cycle 134. A small annular eclipse will cover only 93.71% of the Sun in a very broad path, 262 km wide at maximum, and will last 7 minutes and 54 seconds. Occurring only 4 days after apogee, the Moon's apparent diameter is smaller.
A total solar eclipse will occur on Monday, May 1, 2079, with a maximum eclipse at 10:48:25.6 UTC. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. The eclipse will be visible in Greenland, parts of eastern Canada and parts of the northeastern United States.
An annular solar eclipse will occur on Friday, November 4, 2078. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. The path of annularity will cross Pacific Ocean, South America, and Atlantic Ocean. The tables below contain detailed predictions and additional information on the Annular Solar Eclipse of 4 November 2078.
A total solar eclipse will occur on October 4, 2089. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. The tables below contain detailed predictions and additional information on the Total Solar Eclipse of 4 October 2089.
