Total lunar eclipse february 2 2020 astrology

Some of my own friends loved it so much that they vowed to travel in order to see all future solar eclipses in the U. One even went down to Chile to see the solar eclipse that happened earlier this summer.


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But a lunar eclipse, specifically, is a bit different. For one, a lunar eclipse can be seen almost entirely in the half of the Earth that is experiencing night. And you'll be able to see the next eclipse which is Penumbral on January 10th, But before we dive into exactly how eclipses work—and how and where you can see it—let's delve into a little bit of science, plus everything else we know about when the next lunar eclipse will take place.

All eclipses happen because of the interactions between the sun, moon, and Earth. What makes a lunar and solar eclipse different is, surprisingly, the position of the moon. In August , a huge chunk of America saw a total solar eclipse, which is when the moon moves between the Earth and the sun to block out the sun from view.

In a lunar eclipse, though, the moon is in a different position. A lunar eclipse happens because the Earth comes between the sun and the moon in such a way that the shadow of our planet is either partially or entirely covering our view of the moon—hence the lunar eclipse. It's rare because the moon has to be in just the right part of its orbit for this to happen—and, yes, it can only happen when the moon is full. It might be a bit confusing to learn, but the three different types of lunar eclipses are: Penumbral, partial, and total.

The most recognizable lunar eclipse type is the total eclipse, which happens when the entire moon passes through the Earth's umbral shadow.

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In this case, the moon appears red or orange to us humans below—but more on that later. Meanwhile, a partial lunar eclipse is when a portion of the moon passes through the Earth's umbral shadow and it basically looks like a large part of the moon is covered by a shadow. Here's where things get even more complicated: A Penumbral eclipse happens when the moon passes through the Earth's Penumbral shadow.

In this type of eclipse, none of the moon is completely shaded by the Earth's umbra which is the fully shaded inner region of a shadow. This is the weakest type of eclipse—but still a pretty cool one to see if you can spot it. You already know that a total lunar eclipse is when the moon passes completely under the Earth's umbral shadow. However, the moon doesn't completely disappear.

Instead, it appears completely, just in shadows—and is hard to see if you are not looking for the eclipse, according to Space. When a moon appears red during a total lunar eclipse sometimes referred to as a blood moon , it looks even more mystical than when it is just in shadows. However, this can happen during the total portion of an eclipse because, while the moon is in complete shadow, a bit of light passes from the sun through the Earth's atmosphere, and the colors make the moon look red.

It's a pretty cool effect, but unfortunately, it will be a few years until we may see that again. Typically, there are at least two lunar eclipses per year, but they vary in how strong they are. Because of the three different types of eclipses, no one lunar eclipse is alike. For example, the last total lunar eclipse was in January , and we won't get to see another total lunar eclipse in the U.

However, don't lose hope. Because they do happen often and can be visible to a larger part of the world, you will likely be able to spot the next lunar eclipse long before then. If you missed the recent partial lunar eclipse that happened on July 19, , don't fret. In this particular case, the Moon passes deeply into the umbral shadow leading to a relatively long total eclipse lasting 1 hour 2 minutes.

The times of the major eclipse phases are listed as follows. At the instant of greatest eclipse [1] UT1 the Moon lies at the zenith for a point near eastern Cuba. The umbral eclipse magnitude [3] peaks at 1.

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As a result, the southern half of the Moon will appear much darker than the northern half because the Moon samples a large range of umbral depths during the total phase. The exact brightness distribution in the umbra is difficult to predict, so observers are encouraged to estimate the Danjon value at mid-totality see Danjon Scale of Lunar Eclipse Brightness. It may also be necessary to assign different Danjon values to different portions of the Moon e.

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Much of the eclipse will be seen in central and eastern Europe, but observers there will miss the later stages of the eclipse because they occur after moonset. Likewise parts of the central Pacific experience moonrise after the eclipse begins. Table 2 lists predicted umbral immersion and emersion times for 25 well-defined lunar craters.

The timing of craters is useful in determining the atmospheric enlargement of Earth's shadow see Crater Timings During Lunar Eclipses.


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The January 21 eclipse is the 27th eclipse of Saros This series began on Apr 01 and is composed of 72 lunar eclipses in the following sequence: 8 penumbral, 10 partial, 26 total, 10 partial, and 18 penumbral eclipses Espenak and Meeus, a. In this context, the January 21 eclipse is the 9th total eclipse in the series. The last total eclipse is on Jul 26 and the final eclipse of the series is on May Complete details for this Saros series can be found at: Saros Click for detailed diagram Total Solar Eclipse of July The eagerly awaited total solar eclipse of July 02 is the first one since the Great American Total Eclipse of Such a close Moon during a total eclipse typically produces a long duration of totality - especially if the path passes near the Equator.

In the case of the July 02 event, the maximum duration is just over 4. The total eclipse is visible from within a narrow corridor that traverses the Pacific Ocean and southern South America. A partial eclipse is seen within the much broader path of the Moon's penumbral shadow, which includes the Pacific Ocean and most of South America Figure 3.

Oeno Island is a remote coral atoll and is part of the Pitcairn Islands. Unfortunately, there is no other landfall along the entirety of the Pacific track of kilometers. The region enjoys especially dry and clear weather - so much so that a string of major international astronomical observatories have been built there, including Cerro Tololo, La Silla and Gemini South.

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After crossing the Andes, the lunar shadow descends into Argentina for the last segment of its track. The shadow covers the kilometer-stretch across Argentina in only 3 minutes. In Argentina, San Juan lies just inside the southern limit while Cordoba is 75 kilometers north of the track. Just before the path ends, it barely misses Buenos Aires, the northern edge only 30 kilometers south of the center of the capital. Nevertheless, all roads leading from Buenos Aires to the central line will probably be clogged with traffic on eclipse day. At UT1 the lunar shadow lifts off Earth and returns to space.

Central line coordinates and circumstances are presented in Table 3. Partial phases of the eclipse are visible across the southern Pacific Ocean and South America. Local circumstances for a number of cities in South America are found in Table 4.

The Sun's altitude and azimuth, the eclipse magnitude and obscuration are all given at the instant of maximum eclipse at each location. The Jul 02 Solar Eclipse Circumstances Calculator is an interactive web page that can quickly calculate the local circumstances for the eclipse from any geographic location not included in Table 4. This is the 58th eclipse of Saros Espenak and Meeus, All eclipses in the series occur at the Moon's ascending node and gamma decreases with each member in the family.

The series is a mature one that began with a modest partial eclipse on Oct After 20 partial eclipses in the series and more than 3 centuries, the first umbral eclipse occurred on May The event was a 2-minute total eclipse through New England, eastern Canada and Greenland.

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During the next 2 centuries, the umbral duration continued to increase as each path shifted progressively southward. The greatest umbral duration of Saros occurred during the total eclipse of Aug Unfortunately, the 5 minute 40 second total eclipse was only visible from equatorial Africa, which was virtually inaccessible to astronomers of the day. As the duration of each succeeding eclipse decreased, the paths reversed their southern migration and drifted northward during the 18th and 19th centuries. This effect occurred as a result of the Northern Hemisphere season shifting from winter to summer when the Northern Hemisphere tipped towards the Sun.

The southbound trend of the Saros series resumed with the eclipse of May At this point, the duration of totality at greatest eclipse had again increased to over 5 minutes. The most recent member occurred on Jun 21 and its path crossed southern Africa on the summer solstice. After , the next member occurs on Jul 13 and passes through Australia and New Zealand.

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On Jul 24, the series returns to the African continent producing a path through South Africa. The duration of totality drops as Saros continues to produce total eclipses during the 21st century. The last total eclipse of the series occurs on Aug 15 and lasts a maximum of 1 minute 38 seconds.