Introduction

A total eclipse of the Moon occurs during the early morning hours of October 8, 2014 and is visible from much of North and South America, the Pacific and Australia. Observers in western North America, Hawaii, Japan, New Zealand and eastern Australia will see the entire event. Central and eastern North America will see the beginning stages of the eclipse before moonset while eastern Asia and western Australia witness the later stages after moonrise.

During a total lunar eclipse, the Moon's disk can take on a dramatically colorful appearance from bright orange to blood red and more rarely dark brown to very dark gray. One of the great things about lunar eclipses is that they are completely safe to view with the naked eye. No special filters are required to protect your eyes like those used for solar eclipses. You don't even need a telescope to watch the eclipse, although a good pair of binoculars will help.

An eclipse of the Moon can only take place at Full Moon, and only if the Moon passes through some portion of Earth's shadow. The shadow is actually composed of two cone-shaped parts, one nested inside the other. The outer shadow or penumbra is a zone where Earth blocks some (but not all) of the Sun's rays. In contrast, the inner shadow or umbra is a region where Earth blocks all direct sunlight from reaching the Moon.

When only part of the Moon passes through the umbra, a partial lunar eclipse is seen. If the entire Moon passes through the umbral shadow, then a total eclipse of the Moon occurs. It is also possible to have an eclipse where the Moon passes through only the penumbra. Each of these three eclipses has a unique appearance (see Visual Appearance of Lunar Eclipses). For more information on the how, what, why, when and where of lunar eclipses, see the special web page Lunar Eclipses for Beginners.

Visit Eclipses During 2014 for a complete report on all eclipses occurring over the year.

Path of the Moon through Earth's umbral and penumbral shadows
during the Total Lunar Eclipse of October 8, 2014.
This version of the diagram gives times in Eastern Daylight Time.
(click for larger diagram)

Lunar Eclipse Diagrams

The following diagrams (in high resolution) show the Moon's path through Earth's shadows during October's eclipse. The times of major eclipse stages are given for time zones throughout North America. Please choose the diagram for your own time zone. Each diagram is a GIF file with a size of about 60 KB.

• Eclipse Diagram for GMT (Greenwich Mean Time)
• Eclipse Diagram for EDT (Eastern Daylight Time)
• Eclipse Diagram for CDT (Central Daylight Time)
• Eclipse Diagram for MDT (Mountain Daylight Time)
• Eclipse Diagram for PDT (Pacific Daylight Time)
• Eclipse Diagram for AKDT (Alaska Daylight Time)
• Eclipse Diagram for HST (Hawaiian Standard Time)

The diagrams above of the Total Lunar Eclipse of October 8, 2014 by Fred Espenak, www.EclipseWise.com are licensed under a Creative Commons Attribution-NonCommercial-NoDerivs 3.0 Unported License.

From the eastern and central USA and Canada (time zones ADT, EDT and CDT), the eclipse is still in progress at sunrise as the Moon sets in the west. From the western USA, Canada, Alaska and Hawaii (time zones MDT, PDT, AKDT, and HST), the eclipse begins during the early morning hours of October 8 and ends before the Moon sets. For observers in Hawaii (time zone HDT), entire eclipse occurs on the evening of April 14.

Some people may be puzzled that the Moon's motion in these diagrams is from west to east (right to left), instead of its daily east to west (left to right) motion across the sky. However, the Moon actually moves WEST to EAST (right to left in the Northern Hemisphere) with respect to the Earth's shadow and the stars. At the same time, the Moon, Earth's shadow and the stars all rise in the east and set in the west.

April 15, 2014 Lunar Eclipse Sequence
The total lunar eclipse of April 15, 2014 was widely visible from the USA.
This sequence of images captures the eclipse from start (right) to finish (left).
(click to see larger image)

Times and Phases of October's Total Lunar Eclipse

From start to finish, October's lunar eclipse lasts about three hours and twenty minutes (not including the penumbral phases which are very difficult to see). The partial eclipse begins as the Moon's eastern edge slowly moves into the Earth's umbral shadow. During the partial phases, it takes just over forty minutes for the Moon's orbital motion to carry it entirely within the Earth's dark umbra.

The color and brightness of the totally eclipsed Moon can vary considerably from one eclipse to another. Dark eclipses are caused by volcanic gas and dust which filters and blocks much of the Sun's light from reaching the Moon. Although Indonesia's Mount Kelud has undergone recent volcanic eruptions, it has not produced enough dust and gas to significantly darken October's eclipse. Expect the total phase to appear bright red or orange, which is typical (see: What Will 2014's Lunar Eclipses Look Like?). After the total phase ends, it is once again followed by a partial eclipse as the Moon gradually leaves the umbral shadow. The Visual Appearance of Lunar Eclipses describes what each of these eclipse phases looks like.

The total phase of a lunar eclipse is called totality. At this time, the Moon is completely immersed within Earth's dark umbral shadow. During the October 8 eclipse totality will last nearly 59 minutes. This is a bit shorter than the USA's last total lunar eclipse on April 15, 2014 which lasted 77 minutes.

The major phases of the eclipse occur as follows (all times are GMT or Greenwich Mean Time). The partial eclipse commences with first umbral contact at 09:15 GMT. Totality begins at 10:25 GMT and lasts until 11:24 GMT. The partial phases end at 12:34 GMT. Eclipse times for time zones in the United States and Canada are shown in the following table. Most areas of the United States currently observe Daylight Saving Time (DST). Two notable exceptions are Arizona (although the Navajo Nation does observe Daylight Saving Time) and Hawaii. For observers in Arizona, use the times listed under Pacific Daylight Time (PDT).

The table above provides times of the major eclipse phases for North American time zones and Greenwich Mean Time (GMT). Eclipse times for other time zones can be calculated by taking the difference between local time and Greenwich and adding it to the tabulated GMT times. For more information, see Time Zones. (Note: Although GMT is still in common use, it has actually been replaced by Coordinated Universal Time (UTC), which is based on atomic time.)

To determine the Moon's altitude at each stage of the eclipse as seen from your city or location, see Javascript Lunar Eclipse Explorer. This web page allows you to calculate the viewing circumstances of all lunar eclipses visible from your city over a five-thousand year period.

Visibility of the Total Lunar Eclipse of October 8, 2014

October's lunar eclipse is well placed for western North America, Hawaii, Japan, New Zealand and eastern Australia where the entire event will be visible. Observers in eastern North America and South America will miss some stages of the eclipse because they occur after moonset. Similarly, observers in eastern Asia, the Philippines, and western Australia will miss the early stages of the eclipse since it begins before moonrise. No part of the eclipse is visible from Europe, Africa, or the Middle East.

Preceeding and following the eclipse are hour-long penumbral phases but these are faint and quite difficult to see. The more interesting and photogenic partial and total phases always take center stage to the penumbral phases (see The Pale Penumbral Phase).

Map showing the global visibility of the Total Lunar Eclipse of October 8, 2014.
(Click here to see larger version of this map)

The Visibility Map above for the Total Lunar Eclipse of October 8, 2014 by Fred Espenak, www.EclipseWise.com is licensed under a Creative Commons Attribution-NonCommercial-NoDerivs 3.0 Unported License.

The map above shows the geographic regions of visibility for each phase of the eclipse. The entire eclipse is visible from start to finish in the white (unshaded) portion of the map, while none of the eclipse can be seen from the dark gray areas.

For anyone located in the light gray shaded region labeled Eclipse at Moonset, this means that the Moon will set while some phase of the eclipse is in progress. The contact curves labeled U1, U2, U3, and U4 represent each phase of the eclipse (see the key above). If you are east (right) of a particular curve, that phase occurs after moonset and you will not see it. However, if you are west (left) of a curve, that phase occurs before moonset and you will see it (weather permitting).

For example, on the above map Ohio and Illinois bot lie west (left) of the U3 curve (total eclipse ends) and east (right) of the curve U4 (partial eclipse ends). This means that from this region, the Moon sets during the partial phases following totality.

For observers located within the second light gray shaded region labeled Eclipse at Moonrise, the situation is reversed. Here the Moon rises while some phase of the eclipse is already in progress. If you are west (left) of a particular curve (U1, U2, U3, or U4), that phase occurs before moonrise and you will not see it. However, if you are east (right) of a contact curve, that phase occurs after moonrise and you will see it (weather permitting).

All total eclipses begin with penumbral and partial phases before totality. After the total phase, the eclipse ends with more partial and penumbral phases. Since the penumbral phases of the eclipse are so difficult to see, we will ignore them.

The Total Lunar Eclipse of July 16, 2000 was a very long total eclipse (1 hour 47 minutes)
that won't be exceeded for over a thousand years.
(click for larger image)

Wonderful Totality

At the instant of mid-totality (10:55 GMT), the Moon will lie in the zenith for observers in the South Pacific Ocean about 1200 miles (2000 km) southwest of Hawaii. At this time, the umbral eclipse magnitude peaks at 1.1659. Eclipse magnitude is the fraction of the Moon's diameter immersed in Earth's umbral shadow at greatest eclipse. This value is always 1.0 or larger for total eclipses.

From the eclipse diagrams shown earlier, it is clear that the southern (bottom) edge of the Moon will dip much deeper into the Earth's shadow than will the northern (top) edge. Since Earth's umbral shadow is darker in the center than at the edge, the Moon's appearance will likely change dramatically with time as the total phase progresses. A large variation in shadow brightness can be expected and observers are encouraged to estimate the Danjon value at different times during totality (Danjon Brightness Scale).

This could be an excellent opportunity for budding astronomers and students to test their observing skills. Try recording your estimates of the Moon's brightness every ten minutes during totality using the Danjon Brightness Scale. Compare your results with your companions and classmates and discover how the Moon's appearance changes during the total eclipse. The brightness of the totally eclipsed Moon is very sensitive to the presence of volcanic dust in Earth's atmosphere. As part of a continuing research project, Dr. Richard Keen has been using reports of lunar eclipse brightnesses to calculate a history of optical thicknesses of volcanic dust layers (see: What Will the 2014 and 2015 Lunar Eclipses Look Like?). If you'd like to help Dr. Keen by making eclipse observations, you can contact him .

The amount of dust and sulfur dioxide in Earth's atmosphere also has an effect on the diameter of the umbral shadow. Amateur astronomers with telescopes can make careful timings of when some of the Moon's major craters enter or exit the umbra. Such observations are valuable in determining the enlargement of Earth's shadow. A table of crater predictions identifies twenty well-defined craters useful for this purpose. For more information, see: Crater Timings During Lunar Eclipses.

An eclipse of the Moon also presents a tempting subject to photograph. Since the Moon appears quite small in the sky, you'll need a fairly powerful telephoto lens (400 mm or more) or even a small telescope to attach to your camera. A typical ISO 400 speed (either digital or film) is a good choice. For more information on equipment, film, recommended exposures and additional tips, see How to Photograph a Lunar Eclipse.

Unlike solar eclipses, lunar eclipses are completely safe to watch. Protective filters are not necessary and neither is a telescope. A lunar eclipse can be observed with nothing more than the naked eye. However, a pair of binoculars will magnify the view and make the red coloration brighter and easier to see. A standard pair of 7x35 or 7x50 binoculars is sufficient.

During the eclipse, the Moon will be at its descending node in Pisces. The planet Uranus (visual magnitude = +5.7) lies just 2/3° southeast of the Moon during totality. A pair of binoculars will be a big help in picking out the pale green planet. Is a transit of the Earth and Moon across the Sun's disk visible from Uranus during the eclipse? An interesting idea but calculations show a miss. From Uranus, the Sun's disk is only 1.7 arc-minutes in diameter and this is a very small target to hit. Nevertheless, transits of Earth from Uranus are possible - the next one takes place on 2024 November 17 (Meeus, 1989).

Although total eclipses of the Moon are of limited scientific value, they are remarkably beautiful events which do not require expensive equipment. They help to cultivate interest in science and astronomy in children and to provide a unique learning opportunity for families, students and teachers. To the nature lover and naturalist, the lunar eclipse can be appreciated and celebrated as an event which vividly illustrates our place among the planets in the solar system. The three dimensional reality of our universe comes alive in a graceful celestial ballet as the Moon swings through Earth's shadow. Hope for clear skies, dress warmly and enjoy the show!

The Pale Penumbral Phase

The penumbral phases of the eclipse have been mentioned several times as being difficult to see. In fact, the start of the penumbral eclipse (at 8:16 GMT) is impossible to see. Even when half of the Moon's disk is immersed in the pale penumbral shadow, no trace of it is visible with or without a telescope. This is why the penumbral phases of the eclipse have been downplayed here.

You'll have to wait until about 2/3 of the Moon's disk is in the penumbra before the first hint of the shadow becomes visible (about 8:50 GMT). It is a very diffuse and subtle shading that gradually grows stronger in time. About ten minutes before the partial phase begins (10:15 GMT), the penumbral shading is much more apparent, but the Moon's disk is only diminished slightly in brightness.

The most interesting stage of the penumbral phase is during the last two minutes just before the edge of the Moon's disk begins to enter the umbral shadow (the start of the partial eclipse). Now the penumbral shading is apparent even to the naked eye. Still, this stage of the eclipse literally pales in comparison to the dynamic partial phases and the gloriously beautiful totality.

After totality and the partial phases end (12:34 GMT), the penumbral phases occur in reverse. The Moon exits the penumbra at 13:34 GMT but no trace of the shadow is visible to mark the event.

To get an idea of what to expect during the deeper penumbral phases, see Visual Appearance of Lunar Eclipses.

Total Lunar Eclipses of 2014-2015
Total Lunar Eclipse of 2014 Apr 15	Total Lunar Eclipse of 2014 Oct 08	Total Lunar Eclipse of 2015 Apr 04	Total Lunar Eclipse of 2015 Sep 28

Click on any of the above figures for a closer look.

Tetrads: Four Consecutive Total Lunar Eclipses

October's eclipse is the second to two total lunar eclipses in 2014. The first eclipse was on on April 15 and it was widely visible from all of the USA. In the case of the October 8 eclipse, the western USA sees the entire eclipse while the eastern USA misses the end because the Moon sets while the eclipse is still in progress.

These two eclipses of are the first of four consecutive total lunar eclipses (each separated by six months) - a series known as a tetrad. The third and fourth eclipses of the tetrad occur on April 04, 2015 and Sept. 28, 2015 .

During the 5000-year period from 2000 BCE through 3000 CE, there are 3479 total lunar eclipses. Approximately 16.3% (568) of all total eclipses belong to one of the 142 tetrads occurring over this period. The mechanism causing tetrads involves the eccentricity of Earth's orbit in conjunction with the timing of eclipse seasons. During the present millennium, the first eclipse of every tetrad occurs during the period February to July. In later millennia, the first eclipse date gradually falls later in the year because of precession.

Italian astronomer Giovanni Schiaparelli first pointed out that the frequency of tetrads is variable over time. He noticed that tetrads were relatively plentiful during one 300-year interval, while none occurred during the next 300 years. For example, there are no tetrads from 1582 to 1908, but 17 tetrads occur during the following 2 and 1/2 centuries from 1909 to 2156. The ~565-year period of the tetrad "seasons" is tied to the slowly decreasing eccentricity of Earth's orbit. Consequently, the tetrad period is gradually decreasing (Meeus, 2004). In the distant future when Earth's eccentricity is 0 (about 470,000 years from now), tetrads will no longer be possible.

The umbral magnitudes of the total eclipses making up a tetrad are all relatively small. For the 300-year period 1901 to 2200, the largest umbral magnitude of a tetrad eclipse is 1.4251 on 1949 Apr 13. For comparison, the magnitudes of some other total eclipses during this period are much larger. Two examples are the total eclipses of July 16, 2000 and June 26,2029 with umbral magnitudes of 1.7684 and 1.8436, respectively.

The table below gives the dates of each eclipse in the 8 tetrads occurring during the 21st century. The last tetrad prior to 2014 was in 2003-04 while the next group is in 2032-33.

Two catalogs have been prepared, each listing all tetrads over 3000-year periods:

• Catalog of Lunar Eclipse Tetrads: -2999 to 0000 (3000 BCE to 1 BCE)
• Catalog of Lunar Eclipse Tetrads: 0001 to 3000 (1 CE to 3000 CE)

This multiple exposure sequence shows both partial and total phases of the Total Lunar Eclipse of January 21, 2000.
(click for larger image)

Eclipse Frequency and Future Eclipses

During the five millennium period from 2000 BCE through 3000 CE, there are 7,718 eclipses [1] of the Moon (including both partial and total eclipses). From 0 to 3 lunar eclipses (partial or total) occur each year. The last time three total lunar eclipses occurred in one calendar year was in 1982. On average, partial eclipses slightly outnumber total eclipses by 7 to 6 [2].

The last total lunar eclipse visible from the entire continental United States occurred on April 15, 2014. North Americans will have their next opportunity to see a total lunar eclipse on April 4, 2015. Visit Eclipses During 2014 for a complete report on all eclipses occurring over the year.

The table below lists every lunar eclipse from 2014 through 2020. Click on the eclipse Date to see a description, map and diagram of an eclipse. Although penumbral lunar eclipses are included in this list, they are usually quite difficult to observe because of their subtlety. The penumbra is a partial shadow that permits some direct sunlight to reach the Moon.

The Umbral Eclipse Magnitude is the fraction on the Moon's diameter immersed in the umbra at maximum eclipse. Partial eclipses have a magnitude less than 1. For magnitudes of 1 or greater, the eclipse is total. For negative magnitudes, the eclipse is penumbral. The Eclipse Duration is the duration of the entire eclipse. For total eclipses the duration of the total phase is also listed in bold.

Footnotes

[1] Only eclipses where the Moon passes through Earth's umbral shadow are included in these values. A minor type of eclipse is the penumbral eclipse, which occurs when the Moon passes through the Earth's faint penumbral shadow. Penumbral eclipses are rarely discernible to the naked eye and are of lesser importance than umbral eclipses.

[2] Penumbral eclipses are excluded from these statistics.

Geographic abbreviations (used above): n = north, s = south, e = east, w = west, c = central

The Total Lunar Eclipse of July 16, 2000 as seen from Maui.
(click for larger image)