1  The longest total solar eclipse of the century occurred on July 22 over India, Nepal, Bhutan, and China. It peaked over the Pacific Ocean, but even there the darkness lasted a mere 6 minutes and 29 seconds.

2  Fast and furious: The moon’s shadow zooms across Earth’s surface at up to 5,000 miles per hour.

3  Canadian astronomer and renowned eclipse chaser J. W. Campbell traveled the world for 50 years trying to see 12 different eclipses. He ran into overcast skies every time.

4  Don’t repeat J. W.’s mistakes: Monsoon season throughout south Asia means that there is a good chance the eclipse this July will be clouded out too.

5  Just before full eclipse, dazzling “Baily’s beads” appear where sunlight shines through valleys on the moon. The last bead creates the impression of a diamond ring in the sky.

6  On eclipse-viewing expeditions, this phenomenon is frequently accompanied by a marriage proposal.

7  The beautiful symmetry of a total solar eclipse happens because—by pure chance—the sun is 400 times larger than the moon but is also 400 times farther from Earth, making the two bodies appear the exact same size in the sky.

8  In case you were thinking about relocating: Earth is the only place in the solar system where that happens.

9  Other planets get other kinds of fun, though. Jupiter can have a triple eclipse, in which three moons cast shadows on the planet simultaneously. The event is easily visible through a backyard telescope.

10  The Chinese word for solar eclipse is shih, meaning “to eat.” In ancient China people traditionally beat drums and banged on pots to scare off the “heavenly dog” believed to be devouring the sun.

11  Then again, China also produced the first known astronomical recordings of solar eclipses, inscribed in pieces of bone and shell called “oracle bones,” from around 1050 B.C. or earlier.

12  By comparing those ancient records with modern calculations of eclipse patterns, scientists have determined that the day is 0.047 second longer today than it was back then.

13  Tidal friction, which causes that lengthening of the day, is also making the moon drift away. In about 600 million years it will appear too small to cover the sun, and there will be no more total solar eclipses.

14  In any given location, a total solar eclipse happens just once every 360 years on average.

15  Luckiest place on Earth Carbondale, Illinois, will beat the odds: Folks there will see an eclipse on August 21, 2017, and again on April 8, 2024.

16  In contrast, everyone on the night side of the world can see a lunar eclipse, where the moon slips into Earth’s shadow.

17  During a total lunar eclipse, the moon takes on a deep reddish hue due to the sunlight filtering through our atmosphere—the cumulative glow of all the world’s sunsets.

18  While stranded in Jamaica, Christopher Columbus was famously saved by the lunar eclipse of February 29, 1504, which he had read about in his almanac. After a fracas with the locals, Columbus warned that the moon would disappear if they did not start supplying his men with food.

19  When the moon vanished, the locals promptly complied, and Columbus breathed a huge sigh of relief: His almanac was calibrated for Germany, and he was not sure that he had adjusted correctly for local time.

20  Who knows—it might be useful to you, too. The next lunar eclipse visible from the United States will take place on December 21, 2010.

ECLIPSE of 3-22-1913













The Total Lunar Eclipse of 1913 Mar 22 is visible from the following geographic regions:

  • Asia, Australia, Pacific, Americas

The diagram to the right depicts the Moon’s path with respect to Earth’s umbral and penumbral shadows. Below it is a map showing the geographic regions of eclipse visibility. Click on the figure to enlarge it. For an explanation of the features appearing in the figure, see Key to Lunar Eclipse Figures.

The instant of greatest eclipse takes place on 1913 Mar 22 at 11:57:49 TD (11:57:34 UT1). This is 1.0 days after the Moon reaches perigee. During the eclipse, the Moon is in the constellation Virgo. The synodic month in which the eclipse takes place has a Brown Lunation Number of -121.

The eclipse belongs to Saros 121 and is number 50 of 84 eclipses in the series. All eclipses in this series occur at the Moon’sdescending node. The Moon moves northward with respect to the node with each succeeding eclipse in the series and gammaincreases.

This total eclipse is central meaning the Moon’s disk actually passes through the axis of Earth’s umbral shadow. It has anumbral eclipse magnitude of 1.5683, and Gamma has a value of 0.1671. Because they are so deep, such eclipses typically have the longest total phases. In this case, the duration of totality lasts 92.8 minutes.

The total lunar eclipse of 1913 Mar 22 is followed two weeks later by a partial solar eclipse on 1913 Apr 06.

These eclipses all take place during a single eclipse season.

The eclipse predictions are given in both Terrestrial Dynamical Time (TD) and Universal Time (UT1). The parameter ΔT is used to convert between these two times (i.e., TD = UT1 + ΔT). ΔT has a value of 14.8 seconds for this eclipse.

The following links provide maps and data for the eclipse.

The tables below contain detailed predictions and additional information on the Total Lunar Eclipse of 1913 Mar 22 .

Eclipse Data: Total Lunar Eclipse of 1913 Mar 22

Eclipse Characteristics
Parameter Value
Penumbral Magnitude 2.53401
Umbral Magnitude 1.56828
Gamma 0.16714
Epsilon 0.1698°
Opposition Times
Event Calendar Date & Time Julian Date
Greatest Eclipse 1913 Mar 22 at 11:57:48.9 TD (11:57:34.1 UT1) 2419848.998311
Ecliptic Opposition 1913 Mar 22 at 11:56:05.7 TD (11:55:50.9 UT1) 2419848.997117
Equatorial Opposition 1913 Mar 22 at 11:48:08.9 TD (11:47:54.1 UT1) 2419848.991599
Geocentric Coordinates of Sun and Moon
1913 Mar 22 at 11:57:48.9 TD (11:57:34.1 UT1)
Coordinate Sun Moon
Right Ascension 00h04m39.0s 12h04m58.8s
Declination +00°30’15.3″ -00°21’21.1″
Semi-Diameter 16’02.7″ 16’36.9″
Eq. Hor. Parallax 08.8″ 1°00’58.7″
Geocentric Libration of Moon
Angle Value
l 2.0°
b -0.2°
c 21.9°
Earth’s Shadows
Parameter Value
Penumbral Radius 1.2964°
Umbral Radius 0.7615°
Prediction Paramaters
Paramater Value
Ephemerides JPL DE406
ΔT 14.8 s
Shadow Rule Danjon
Shadow Enlargement 1.010
Saros Series 121 (50/84)

Explanation of Lunar Eclipse Data Tables

Eclipse Contacts: Total Lunar Eclipse of 1913 Mar 22

Lunar Eclipse Contacts
Eclipse Event Contact Time
Zenith Latitude Zenith Longitude Position Angle Axis Distance
Penum Begins P1 09:17:56.8 09:17:42.0 00°27.0’N 138°55.2’W 305.3° 1.5740°
Partial Begins U1 10:13:05.5 10:12:50.7 00°10.3’N 152°14.2’W 308.5° 1.0389°
Total Begin U2 11:11:25.3 11:11:10.5 00°07.3’S 166°19.4’W 319.6° 0.4847°
Great Eclipse Great 11:57:48.9 11:57:34.1 00°21.4’S 177°31.6’W 29.1° 0.1698°
Tot Ends U3 12:44:11.9 12:43:57.1 00°35.4’S 171°16.2’E 98.6° 0.4845°
Partial Ends U4 13:42:31.3 13:42:16.5 00°53.0’S 157°11.1’E 109.7° 1.0379°
Penum Ends P4 14:37:43.4 14:37:28.7 01°09.6’S 143°51.2’E 112.9° 1.5725°
Eclipse Durations
Eclipse Phase Duration
Penumbral (P4 – P1) 05h19m46.7s
Partial (U4 – U1) 03h29m25.8s
Total (U3 – U2) 01h32m46.6s

Explanation of Lunar Eclipse Contacts Table

Polynomial Besselian Elements: Total Lunar Eclipse of 1913 Mar 22

Polynomial Besselian Elements
1913 Mar 22 at 12:00:00.0 TD (=t0)
n x y d f1 f2 f3
0 0.10131 0.13799 0.0088 1.29635 0.76149 0.27692
1 0.51285 -0.28558 0.0003 -0.00023 -0.00022 -0.00006
2 -0.00012 0.00006 -0.0000 -0.00000 -0.00000 -0.00000
3 -0.00001 0.00001

At time t1 (decimal hours), each besselian element is evaluated by:

x = x0 + x1*t + x2*t2 + x3*t3 (or x = Σ [xn*tn]; n = 0 to 3)

where: t = t1 – t0 (decimal hours) and t0 = 12.000