How are solar and lunar eclipses formed?
First, the phenomenon of solar eclipse
Eclipses and celestial cones
Eclipses are spectacular astronomical phenomena, but also short-lived and harmless natural phenomena. Its occurrence is related to the shadow of the moon and the earth.
Under the irradiation of the sun, the earth and the moon are dragging long shadows away from the sun. The sun, the earth and the moon are all spheroids, and the sun is much bigger than the earth and the moon. Therefore, the main part of their shadow is a convergent cone with its top facing away from the sun, which is called umbra. In the umbra, all the solar disks are covered, so it is dark (strictly speaking, the umbra of the earth is not completely dark due to the refraction of the atmosphere). Because the sun is a spherical light source, there is a transition zone between light and shade around the umbra. This is a divergent cone much larger than the umbra, called penumbra. In this shadow area, you can get part of the sun's brilliance, so it is not completely dark. In penumbra, the extension line of the umbra cone is an emission cone coaxial with and opposite to the umbra, which is called pseudo-umbra. It is a special penumbra, the central part of the sun's disk is covered, and the edge part of the sun is still visible, so it is not completely dark. Different parts of penumbra and pseudo-umbra have different degrees of light and shade: the closer to umbra, the darker it is; The farther away from the umbra, the less sun gear is covered and the brighter it is.
The length of umbra varies with the size of the projected object and its distance from the sun. The larger the radius of a celestial body, the longer its umbra. The radius of the moon is about 27% that of radius of the earth. If the distance between the moon and the sun is equal, the length of the moon's umbra is also 27% of the earth's umbra. The farther a celestial body is from the sun, the longer its umbra is. In a year, when the earth (and the moon) approaches the perihelion, the umbra becomes longer; Near the perihelion, the umbra is very short. Within a month, before and after the full moon, the umbra of the moon is longer; Around the new moon, the umbra of the moon is shorter.
According to the radii of the sun, the earth and the moon, and the average distance between the sun and the moon, the average length of the earth's umbra is 1377 000km, which is about 3.5 times that of the moon's umbra. At the new moon, the average length of the umbra is 374 500 kilometers, which is slightly less than the average distance between the moon and the earth (384 400 kilometers). Therefore, when the shadow of the moon reaches the earth, it can be the top of the umbra or its pseudo-umbra.
Together, the moon drags its own shadow around the earth. When it reaches the sun surface of the earth, its shadow sometimes sweeps across the ground. At this time, in the area swept by the moon shadow, people see that the sun is covered by the moon wheel, which is called a lunar eclipse. When the moon goes around the earth with its back to the sun, it happens to be hidden in the umbra of the earth. At this time, from the perspective of the earth, the full moon loses its luster in the sky, which is an eclipse. As you can imagine, when an eclipse occurs, what you see in the moon and sky is an eclipse; When there is a solar eclipse on the earth, a small shadow appears on the bright "place" in the night sky of the moon, which can be called "Lingdi".
Types of solar eclipses
There are three kinds of solar eclipses: total solar eclipse, partial solar eclipse and annular solar eclipse, also called annular solar eclipse. Their difference depends on which part of the moon's shadow covers the ground.
As we all know, the diameter of the moon is much smaller than that of the earth. Therefore, the umbra of the moon can only cover a small part of the ground at any time. In this small area, it seems that all the solar disks are covered, which is called a total solar eclipse. If the umbra of the moon was not long enough at that time, it was not the umbra of the moon but its pseudo-umbra that touched the ground. Then, the sun seen in the pseudoumbra is covered by the moon wheel in the middle and the edge is still shining, which is the annular eclipse. It goes without saying that when the umbra or pseudoumbra of the moon falls to the ground, its penumbra will also arrive at the same time. Therefore, there is an annular penumbra around the total solar eclipse or annular solar eclipse area. From there, the sun seems to be partially covered by the moon wheel, and the CD is not complete. This is a partial solar eclipse. In this way, at the same time, total solar eclipse and partial solar eclipse occurred in different parts of the earth; In the same area, there must be a partial eclipse stage before and after the annular eclipse.
Due to the rotation of the moon around the earth and the earth itself, the eclipse zone moves on the ground, forming an eclipse zone. The middle part of the eclipse belt is a total solar eclipse (or annular solar eclipse) belt, and the north and south sides are partial solar eclipse belts. In the process of moving, the distance between the tip of the lunar umbra and the ground changes. Because of this change, it sometimes happens that the beginning and end stages of the solar eclipse are annular eclipses, while the total solar eclipse occurs in the middle stage. This eclipse is called total solar eclipse. Sometimes, due to the deviation of the lunar shadow cone, the solar eclipse belts on the ground are all partial eclipse belts. Such an eclipse will always be a partial eclipse.
Eclipses can be divided into total solar eclipse and partial solar eclipse, and there is no annular solar eclipse. The difference between a total lunar eclipse and a partial lunar eclipse lies in whether the moon is completely or partially hidden in the umbra of the earth, rather than at different observation points on the earth. When the moon is completely hidden in the umbra of the earth, the whole moon wheel becomes dark, which is a total lunar eclipse. If the moon only partially enters the umbra of the earth, then the moon wheel is incomplete and it is a partial solar eclipse. Naturally, before and after the total lunar eclipse, there must be a partial lunar eclipse. Sometimes, because the moon is far away from the umbra axis of the earth, the whole eclipse process is always a partial eclipse. Whether it is a total solar eclipse or a partial solar eclipse, similar eclipses are seen all over the world (night hemisphere) at the same time.
Unlike solar eclipses, lunar eclipses have nothing to do with the penumbra and artifacts of the earth. When the moon enters the penumbra of the earth, the "eclipse" will not happen, because part of the sun's brilliance can be obtained in the penumbra, and it still illuminates the whole surface of the moon, but the brightness becomes slightly darker, and the moon wheel is still indispensable. This phenomenon is called a penumbral eclipse, and the Observatory usually does not give advance notice.
As for why there is no eclipse? The reason is obvious, because at the orbital distance of the moon, the cross section of the umbra is much larger than that of the moon wheel.
Among the above food types, the most rare, spectacular and fascinating is the total solar eclipse. When the total solar eclipse comes, the sky is dark, just like the sudden arrival of night, birds return to their nests, chickens and dogs enter their nests, and animals all show panic. Nothing is more exciting than the dark day of the sun. The most famous total solar eclipse in history (May 28th, 585 BC, in Asia Minor Peninsula, now Turkey) dramatically ended the five-year war between two ethnic tribes and became an interesting episode in the history of war.
The total solar eclipse is also of great scientific significance. This is an excellent opportunity to study the sun. As we know, the brightness of the chromosphere and corona is very weak, and they are completely submerged in the sun at ordinary times. Only when there is a total solar eclipse, the source of atmospheric scattered light is cut off, and the sky is dark, the chromosphere and corona are particularly clear. Astronomers can take this opportunity to capture their spectra (at this time there is no light source behind them to produce Fraunhofer lines); The study of chromosphere and corona is of great significance for exploring the physical state of the sun itself and between the sun and the earth. For example, helium, known as the "solar element", was discovered by astronomers in the chromosphere spectrum taken during the total solar eclipse in 1868, while chemists did not discover it from the analysis of yttrium uranium ore until 1895. At that time, some people praised celestial spectroscopy for running ahead of chemistry. Helium atom is a kind of atom that is difficult to "excite". It needs a high temperature to make it emit visible light. Its spectral line appears in the chromosphere spectrum, indicating that the temperature in the chromosphere of the sun is very high. Some astronomers also use this once-in-a-lifetime opportunity to search for planets in the water and recent comets near the sun. Therefore, whenever there is a total solar eclipse, astronomers always carry heavy instruments and travel long distances to the total solar eclipse area for observation and research in various disciplines.
The process of solar eclipse
The whole process of total solar eclipse can be divided into three stages: partial eclipse-total solar eclipse-partial solar eclipse. These three stages are divided into four food phases: first loss, second food, raw light and last contact. From food to light is the whole food stage; The first loss to food, the second loss to the last contact, is the partial eclipse stage before and after the total solar eclipse.
Both the moon and the sun move eastward on the celestial sphere. The former takes the sidereal moon as the cycle, and the speed is about1310' every day; The latter takes the sidereal year as the cycle and the speed is about 59 feet per day. Obviously, the moon moves much faster than the sun. It chases the sun and the umbra of the earth from west to east at a speed of about1310'-59' =121'every day. In other words, the process of solar eclipse is the process that the moon catches up with the sun eastward on the celestial sphere, thus covering the sun. Therefore, the process of solar eclipse always starts from the western edge of sun gear and ends at the eastern edge. Similarly, the process of an eclipse is that the moon passes the umbra of the earth eastward on the celestial sphere, thus being blocked. Therefore, eclipses always start at the eastern edge of the moon and end at the western edge.
In the process of the moon catching up with the cross section of the shadow of the sun and the earth, the two circular surfaces will be circumscribed and inscribed twice, which are the four eclipse phases above. For the total solar eclipse, the meaning of these four eclipse stages is:
The first loss-the eastern edge of the moon wheel is tangent to the western edge of the same wheel, and the partial solar eclipse begins.
Eclipse-the eastern edge of the moon wheel is inscribed with the eastern edge of the same wheel, and the total solar eclipse begins.
Light-the western edge of the moon wheel is inscribed with the western edge of the same wheel, and the total solar eclipse is over.
The last contact-the western edge of the full moon is tangent to the eastern edge of the full moon, and the partial eclipse ends.
For the total eclipse process, the meaning of these four eclipse stages is:
Initial loss-the eastern edge of the moon wheel is tangent to the western edge of the umbra section at the same place, and the partial eclipse of the moon begins.
Eclipse-the western edge of the moon wheel is inscribed with the western edge of the umbra section, and the total lunar eclipse begins.
Illumination-the eastern edge of the moon wheel is inscribed with the eastern edge of the umbra section of the earth, and the total lunar eclipse ends.
The last contact-the western edge of the moon wheel is tangent to the eastern edge of the umbra section, and the partial eclipse ends.
An annular eclipse also has an eclipse on it. However, it has no total solar eclipse stage. Therefore, although there are two inscribed lines between the sun and the moon, there is no real food and light. It doesn't matter whether the partial eclipse of the sun and the partial eclipse of the moon are light or light.
In the process of solar eclipse and lunar eclipse, the moment when the center of the moon wheel is closest to the center of sun gear or the umbra section of the earth is called an eclipse. The degree to which sun gear or the moon wheel is "eaten" under the condition of heavy food is called food score. The calculation of the food part is based on the apparent diameters of the sun and moon rings. For example, a lunar eclipse of 0. 5 means that 50% (not half) of the diameter of the sun and moon wheels is covered. The score of food with partial eclipse is > 0, <1; The total food score is ≥ L, and in the same solar eclipse, the food score and time can be different in different places; But in the same eclipse, as long as you can see the whole process, the time to eat and see the food is the same.
Conditions of solar eclipse
There are certain conditions for the occurrence of solar and lunar eclipses. If we understand these conditions, people can calculate and predict the occurrence of solar and lunar eclipses. It is an important part of ancient astronomy in China and occupies an important position in the history of world astronomy.
The movement of the moon to catch up with the sun to the east occurs in the process of its respective movement to the west on Sunday, and the specific situation varies with latitude, season and northern and southern hemispheres.
-The equator of the celestial sphere inclines to the south and the north pole of the celestial sphere tilts upward, indicating that it is in the northern hemisphere;
—— The intersection angle between the celestial equator and the horizon map is the local residual latitude, so the latitude is 45° N；; ;
—— The sun's Sunday circle (declination) is south of the celestial equator, so it is winter in the northern hemisphere;
-The sun and the moon are setting towards the western horizon; It can be seen that the time is approaching evening.
Simply put, the condition of solar eclipse is that the earth is located in the back direction of the moon (that is, the direction of the shadow of the moon), so it is located on the extension line connecting the sun and the moon. The condition of an eclipse is that the moon is located in the back direction of the earth (that is, the direction of the shadow), so it is located on the extension line connecting the sun and the earth. For the convenience of explanation, this general condition can be divided into two specific conditions:
-Conditions of the new moon: The solar eclipse will occur in the new moon, and the eclipse will occur in front of us. In the new moon, only on the date of the new moon can the earth be located in the direction of the moon shadow; On the date of the moon, the moon may be in the direction of the shadow. In this way, solar and lunar eclipses are associated with the moon. According to this principle, the calendar was tested by solar eclipse in ancient China. If the solar eclipse does not occur on the first day of the first year, then the calculation of the lunar calendar will definitely become a problem.
-Intersection conditions: the solar eclipse occurs in the new moon, and the eclipse is in sight; However, not every new moon will have an eclipse, and not every moon will have an eclipse. Experience tells us that solar and lunar eclipses will not occur in most areas of Wang Shuo. This is because there is an intersection angle of 5 9' between the ecliptic and the ecliptic (called the intersection angle of yellow and white), and the apparent diameter of the moon and sun gear is only about 0.5. It can be seen that the conditions of an eclipse are only necessary conditions, not sufficient conditions. The new moon (conjunction of the sun and the moon) and hope (collision of the sun and the moon) only indicate that the eclipses of the sun and the moon are the same or different180; However, if they really overlap on the celestial sphere, then their yellow latitudes should be equal (or close). This requires the moon and the sun to be at or near the intersection of yellow and white at the same time. If the sun and the moon meet or collide and are not near the intersection of yellow and white, then at the new moon, the shadow cone of the moon passes through the north and south of the earth and does not touch the ground; The apparent moon also passes through the north and south of the earth's shadow cone and does not enter the umbra of the earth.
Generally speaking, the condition of solar eclipse is that the sun and the moon meet at or near the intersection of yellow and white; The condition of solar eclipse is that the sun and the moon collide (see) into yellow and white.
Food restrictions and seasons
The occurrence of solar and lunar eclipses requires the sun and the moon to meet (or collide) at or near the intersection of yellow and white. This "neighborhood" has a certain limit, that is, the food limit. As far as solar eclipse is concerned, at this limit, the moon wheel on the white road and the sun wheel on the ecliptic are close to each other, and the angular distance between their centers is the sum of their apparent radii, that is, about 32'. At this time, the ecliptic arc length from the center of sun gear to the intersection of yellow and white is called the eclipse limit. As we know, the sun runs along the ecliptic, and its position is represented by the ecliptic; The center of sun gear.
The difference of the yellow meridian at the intersection of yellow and white indicates the limit of solar eclipse, which is directly related to the length of time the sun has experienced. If the sun collides with the moon instead of the sun meets the moon, and the sun gear is replaced by the cross section of the umbra, then such a limit is the eclipse limit. When the sun is tangent to the moon, the arc length of the ecliptic from the intersection of yellow and white to the center of sun gear is the difference between the center of sun gear and the adjacent intersection of yellow and white at this moment.
The size of the food limit depends on the size of the intersection of yellow and white, the distance between the moon and the earth, and the distance between the sun and the earth. These factors are changing: the intersection angle of yellow and white varies from 4 59 ′-518 ′; The distance between the moon and the earth varies between 363,300 km (perigee) and 405,500 km (apogee). The distance between the sun and the earth varies between 147 100 000km (perihelion) and 152 100 000km (apohelion). Therefore, the size of the solar eclipse limit and the solar eclipse limit are also changing. Here, we can't explain their specific size, only their general change law:
-The greater the intersection angle between yellow and white, the smaller the food limit and food limit;
The greater the distance between the moon and the earth, the smaller the apparent radius of the moon wheel, and the smaller the eclipse limit and eclipse limit;
—— The greater the distance between the sun and the earth, the smaller the apparent radius of sun gear and the smaller the solar eclipse limit; However, the apparent radius of the shadow part increases, so the eclipse limit also increases.
Therefore, when the intersection angle of yellow and white, the distance between the moon and the earth and the distance between the sun and the earth are the largest, the solar eclipse limit is the smallest; On the contrary, when all three are the smallest, the solar eclipse limit is the largest. The situation of eclipse limit is different: when the yellow and white intersect, the distance between the moon and the earth is the largest, the distance between the sun and the earth is the smallest, and the eclipse limit is the smallest; On the contrary, when the intersection angle between yellow and white is the smallest and the distance between the moon and the earth is the largest, the eclipse limit is the largest.
The difference between the intersection of the yellow meridian and the yellow meridian in the center of sun gear is less than the minimum eclipse time, and a solar eclipse is bound to occur. Daily (monthly) eclipse may occur if it is greater than the minimum food intake limit but less than the maximum food intake limit; If it is greater than the maximum food limit, there will be no food.
The sizes of solar eclipse boundaries (including partial eclipse and total eclipse) and lunar eclipse boundaries (including penumbra, partial eclipse and total eclipse) are compared as follows:
As can be seen from the above table, the solar eclipse limit is slightly greater than the solar eclipse limit. However, if the penumbral eclipse is excluded, the eclipse limit is much greater than the eclipse limit.
In order to calculate the size of the food limit, besides the apparent radius of the sun and the moon and the intersection angle of the sun and the moon, the geodetic adjustment of the sun and the moon should also be considered.
S, e, m and M' represent the centers of the sun, the earth and the moon, respectively. As far as the eclipse is concerned, when the moon begins to contact the sun gear (initial loss), the opening angle of the center of the sun and the center of the moon to the center of the earth is the yellow latitude of the moon at that time. SEM=∠SEA+∠AEB+∠BEM. Where ∠SEA and ∠BEM are the apparent radii of the sun and the moon, respectively, which are expressed by S⊙ and S-moon; ∠ AEB =∠ CBE —∠ CAE, which are the ground adjustment of the moon and the sun, respectively, expressed by π moon and π ⊙, then there is.
∠ SEM = s ⊙+s Moon-π ⊙+π Moon
For an eclipse, at the initial loss, the moon wheel begins to contact the umbra of the earth (for convenience, the position of the moon is replaced by the last contact). At this time, the yellow latitude of the moon is ∠ tem ′-∠ m ′ ed+∠ det. Where ∠m'ed is the apparent radius s of the moon; And det = CDE-etd. ∠CDE is the earth adjustment of the moon π moon; And ∠ ETD = ∠ AES-∠ CAE, which are solar apparent radius S⊙ and solar-terrestrial adjustment π ⊙ respectively. Then there is:
∠ TEM' = S Moon+π Moon -S ⊙+π⊙
We know that the sun and the moon have similar apparent diameters, with the former averaging 15' 59.6 and the latter averaging 15' 32.6. However, their geodetic adjustment is quite different: the average geodetic adjustment of the sun is only 8. "8, and the average adjustment of the moon is 57' 2". Therefore, ∠SEM >∠TEM'. The greater the latitude of yellow latitude, the farther away from the intersection of yellow and white, and the solar eclipse limit is greater than the lunar eclipse limit.
The food season is a period when solar and lunar eclipses may occur, which is related to food restriction. Because the occurrence of solar and lunar eclipses must meet two conditions at the same time, not all new moons and eclipses can occur. Therefore, solar and lunar eclipses can only occur at certain times of the year. As we know, the conditions of solar eclipse and lunar eclipse are that the sun and the moon must be at the same yellow-white intersection (eclipse), or separated by two yellow-white intersections (eclipse) or close to two yellow-white intersections. Comparatively speaking, the moon passes through the intersection of yellow and white frequently (twice a month), 24.5 times a year; And the sun comes to the intersection once every six months. Therefore, whether there was a solar eclipse or a lunar eclipse at that time mainly depended on whether the sun was located at or near the intersection of yellow and white. The time when the sun exceeds the food limit is called food season. Generally speaking, there are two food seasons in a year, about half a year apart.
The length of the food season mainly depends on the size of the food limit. The greater the food restriction, the longer the food season. According to the size of the food limit and the annual movement speed of the sun (average 59' per day), people can calculate the approximate number of days in the food season. For example, if the minimum food limit of partial solar eclipse is 15.9, then its food season will not be shorter than15.9× 2÷59 ′ = 32.2 days. This length has exceeded the moon. In other words, during this time, the moon will come to the intersection once. So, there must be two eclipses in a year. As it happens, there is an eclipse at the beginning and end of each season, so there are four eclipses a year.
For another example, if the maximum eclipse limit of the partial eclipse is 1 1.9, then its season length will not exceed11.9× 2 ÷ 59 ′ = 24.2 days. This length is less than a full moon. In other words, during this time, the moon may not necessarily come to the intersection. Therefore, there is not even an eclipse in some years; If there is, it can only be once a season, which happens to be twice a year.
Because the intersection of yellow and white recedes to the west by about 20 degrees every year, an intersection year (also called the food year) is only 346.2600 days, which is about 19 days shorter than the tropic year. Therefore, the following two situations may occur:
First of all, there are two complete food seasons and one incomplete food season in a year. If the first food season has just started at the beginning of the year, in addition to the third food season in the middle of the year, the third food season may be ushered in the middle of February1the same year. In this case, there may be five eclipses and two eclipses this year. In the second case, there is a complete food season (the middle of the year) and two incomplete food seasons (the beginning and the end of the year) in a year. In this case, there may be four eclipses and three eclipses.
In the former case, for example, if the first food season starts on June 65438+ 10 1, it coincides with the new moon and a solar eclipse occurs. In the next 346 days (an eclipse year), under the most favorable circumstances, four eclipses and two eclipses may occur in the two eclipse seasons. The third eclipse season begins around 65438+February 12. Because the 12 moon is 354.36 days, which is about 8 days older than the eclipse, the 13 eclipse will not occur until about 65438+February 20, and there may be another eclipse. The remaining date is less than half a month, even if there is an eclipse, it will have to wait until the beginning of the following year 1 month. However, this situation is very rare.
Globally, there are more eclipses than eclipses. But for a place, the number of eclipses is far more than the number of eclipses. This is because during the eclipse, the eclipse area is very wide (it can be seen everywhere in the night hemisphere), while during the eclipse, only a very narrow area can be seen on the earth. According to statistics, for a specific location, a total lunar eclipse can occur every three or four years on average; But the total solar eclipse takes hundreds of years on average to encounter. So many people in the world have never seen a total solar eclipse in their whole lives.
On July 22nd, 2009, China will see a total solar eclipse. The solar eclipse is 230 kilometers wide and 3000 kilometers long, spanning southern Tibet and the Yangtze River basin. The total lunar eclipse lasts 5-6 minutes (the longest total solar eclipse lasts about 7 minutes), which coincides with the sunny and hot weather in midsummer in the south of the Yangtze River, and the observation conditions are excellent. This will be a once-in-a-lifetime opportunity.
Cycle of solar and lunar eclipses
The conditions of solar eclipse and lunar eclipse contain various periodic astronomical factors, so they have strict and complex periodicity. First of all, the solar eclipse will happen in the new moon, and the eclipse will happen in front of us. The first month of the lunar calendar is a period of phase change, and its length is 29.5306 days. Secondly, when an eclipse occurs, the sun must be at or near the intersection of yellow and white. It is a periodic phenomenon that the sun passes through the intersection of yellow and white, and its cycle is the intersection year (food year), which is 346.6200 days Thirdly, when an eclipse occurs, the moon will come to or near the yellow-white intersection at the same time, and the period of the moon passing through the same yellow-white intersection twice in a row is the intersection month, that is, 27.438+022 days. In addition, when the moon approaches perigee, it runs fast; When approaching apogee, the running speed is slow. This difference in distance and speed is also a periodic change, and its period is the latest month, that is, 27.5546 days.
The above four periods are combined into a * * * same period, that is, their least common multiple, which is called Sharo period. Its length is 6585.32 days, equivalent to 223 new months, almost equivalent to 242 intersection months, roughly equivalent to 239 perigee months and 19 food years, as shown in the following table:
Shuowangyue (29.5306 days) × 223 = 6585.32 days.
Nodal month (27.2 122) × 242 = 6585.35.
Recent months (27.5546 days) × 239 = 6585.55 days.
Food year (346.6200 days) × 19 = 6585.78 days.
According to the current Gregorian calendar, the Shaluo period is equivalent to 18 1 1.32 days (if there are five leap years in between, it is 18 and 10.32 days). After such a long time, the relative position of the intersection of the sun, the moon, the yellow and white, and the distance between the moon and the earth have all returned to almost the same situation as before. As a result, the solar eclipse series of the last cycle appeared again. In the Charlotte cycle, the time of solar eclipse and lunar eclipse is roughly equal, and the types of solar eclipse and lunar eclipse are also the same. At the same time, every solar eclipse and lunar eclipse will be repeated after a Charlotte cycle. For example, the annular solar eclipse on September 23rd, 1987 in/kloc-0 will reappear on October 3rd, 2005.
However, because the Charlotte cycle is not an integer multiple of the solar day, two solar eclipses or lunar eclipses corresponding to each other will not occur at the same time in one day. Its mantissa, less than 1 day, is 0.32 days, that is, 1/3 days, which delays the corresponding two eclipses by about 8 hours, so it is about 120 degrees west longitude. For example,1the annular solar eclipse on September 23rd, 987 can be seen in Russia, China and the Pacific Ocean. The annular solar eclipse that will occur on June 3, 2005 10 can be seen in the Atlantic Ocean, Africa and the Indian Ocean. In addition, strictly speaking, the Charlotte period is not equal to an integer multiple of the intersection month, perigee month and solar eclipse year. So the corresponding solar eclipse or lunar eclipse is just similar, but not exactly the same.
In short, the Sharo cycle does not include all the factors related to the same day and solar eclipse. Its simple regularity has no absolute significance, so it cannot replace the specific calculation of solar eclipse.