The Earth's orbit is the trajectory of its rotation around the Sun, its shape is an ellipse, it is located on average at a distance of 150 million kilometers from the Sun (the maximum distance is called aphelion - 152 million km, the minimum - perihelion, 147 million km).

The Earth completes a full revolution around the Sun, 940 million km long, moving from west to east at an average speed of 108,000 km/h in 365 days, 6 hours, 9 minutes and 9 seconds, or one sidereal year.

The movement of the planet in its orbit around the Sun and the angle of inclination of the axis of rotation to the plane where celestial bodies move directly affect the change of seasons and the inequality of day and night.

Features of the Earth's rotation around the Sun

(Structure of the Solar System)

In ancient times, astronomers believed that the Earth was located at the center of the Universe and all celestial bodies revolved around it; this theory was called geocentric. It was debunked by the Polish astronomer Nicolaus Copernicus in 1534, who created a heliocentric model of the world, which proved that the Sun cannot revolve around the Earth, no matter how much Ptolemy, Aristotle and their followers wanted it.

The Earth revolves around the Sun along an elliptical path called an orbit, its length is about 940 million km and the planet travels this distance in 365 days 6 hours 9 minutes and 9 seconds. After four years, these six hours accumulate per day, they are added to the year as another day (February 29), such a year is a leap year.

(Perihelion and aphelion)

During the period of movement along a given trajectory, the distance from the Earth to the Sun can be maximum (this phenomenon occurs on July 3 and is called aphelion or apohelion) - 152 million. km or minimum - 147 million. km (occurs on January 3, called perihelion).

As a result of the Earth's distance and approach to the Sun, due to the inclination of the Earth's axis to the plane of its orbit around the Sun at 66.5º, the Earth's surface receives an unequal amount of heat and light, which causes the change of seasons and changes in the duration of day and night. Equatorial days and nights are always equally long, they last 12 hours.

Speed ​​of the Earth moving in orbit

Earth's revolution around the Sun: 365 days 6 hours 9 minutes and 9 seconds

Average speed of the Earth in its orbit around the Sun: 30 km/s or 108,000 km/h (it's 1/10000th the speed of light)

For comparison, the diameter of our planet is 12,700 km, with this speed it is possible to cover this distance in 7 minutes, and the distance from the Earth to the Moon (384 thousand km) in four hours. Moving away from the Sun during the aphelion period, the Earth's speed slows down to 29.3 km/s, and during the perihelion period it accelerates to 30.3 km/s.

The influence of the Earth's orbit around the Sun on the changing seasons

The angle between the Earth's axis and the plane of the ellipse is 66.3º, and it is the same along the entire length of the orbit. The angle between the plane in which the Earth moves relative to the Sun (called the ecliptic) and its axis of rotation is 26º 26 ꞌ.

(Change of seasons on Earth)

The places where the plane of the celestial equator intersects the plane of the ecliptic are designated by the vernal points ( 21 March) and autumnal equinox ( 23 September), days and nights are equally long, and the areas of the hemispheres facing the Sun are evenly illuminated and warmed, the rays of the Sun fall on the equator line at an angle of 90º. The astronomical beginning of spring and autumn in the corresponding hemispheres is calculated using the dates of the spring and autumn equinoxes.

There are also points of summer ( 22nd of June) and winter ( December 22) solstice, the rays of the Sun become perpendicular not to the equator line, but to the Southern and Northern Tropics (the southern and northern parallels are 23.5º). On the day of the summer solstice, June 22, in the Northern Hemisphere, up to 66.5 parallels, the day is longer than the night, in the Southern Hemisphere, the night is longer than the day, this date is the astronomical beginning of summer in northern latitudes and winter in southern latitudes.

On December 22 (winter solstice day) in the Southern Hemisphere up to the 66.5 parallel the day length is longer, in the Northern Hemisphere up to the same parallel it is shorter. The date of the winter solstice is the astronomical beginning of winter in the Northern Hemisphere and the beginning of summer in the Southern.

Like other planets of the solar system, it makes 2 main movements: around its own axis and around the Sun. Since ancient times, it was on these two regular movements that calculations of time and the ability to compile calendars were based.

A day is the time of rotation around its own axis. A year is a revolution around the Sun. The division into months is also in direct connection with astronomical phenomena - their duration is related to the phases of the Moon.

Rotation of the Earth around its own axis

Our planet rotates around its own axis from west to east, that is, counterclockwise (when viewed from the North Pole.) An axis is a virtual straight line crossing the globe in the area of ​​the North and South Poles, i.e. the poles have a fixed position and do not participate in rotational motion, while all other location points on the earth's surface rotate, and the rotation speed is not identical and depends on their position relative to the equator - the closer to the equator, the higher the rotation speed.

For example, in the Italian region the rotation speed is approximately 1200 km/h. The consequences of the Earth's rotation around its axis are the change of day and night and the apparent movement of the celestial sphere.

Indeed, it seems that the stars and other celestial bodies of the night sky are moving in the opposite direction to our movement with the planet (that is, from east to west).

It seems that the stars are around the North Star, which is located on an imaginary line - a continuation of the earth's axis in a northerly direction. The movement of stars is not proof that the Earth rotates around its axis, because this movement could be a consequence of the rotation of the celestial sphere, if we assume that the planet occupies a fixed, motionless position in space.

Foucault pendulum

Irrefutable proof that the Earth rotates on its own axis was presented in 1851 by Foucault, who conducted the famous experiment with a pendulum.

Let's imagine that, being at the North Pole, we set a pendulum into oscillatory motion. The external force acting on the pendulum is gravity, but it does not affect the change in the direction of oscillations. If we prepare a virtual pendulum that leaves marks on the surface, we can make sure that after some time the marks will move in a clockwise direction.

This rotation can be associated with two factors: either with the rotation of the plane on which the pendulum makes oscillatory movements, or with the rotation of the entire surface.

The first hypothesis can be rejected, taking into account that there are no forces on the pendulum that can change the plane of oscillatory movements. It follows that it is the Earth that rotates, and it makes movements around its own axis. This experiment was carried out in Paris by Foucault, he used a huge pendulum in the form of a bronze sphere weighing about 30 kg, suspended from a 67-meter cable. The starting point of the oscillatory movements was recorded on the surface of the floor of the Pantheon.

So, it is the Earth that rotates, and not the celestial sphere. People observing the sky from our planet record the movement of both the Sun and planets, i.e. All objects in the Universe move.

Time criterion – day

A day is the period of time during which the Earth makes a complete revolution around its own axis. There are two definitions of the concept “day”. A “solar day” is a period of time of the Earth’s rotation, during which . Another concept - “sidereal day” - implies a different starting point - any star. The length of the two types of days is not identical. The length of a sidereal day is 23 hours 56 minutes 4 seconds, while the length of a solar day is 24 hours.

The different durations are due to the fact that the Earth, rotating around its own axis, also performs an orbital rotation around the Sun.

In principle, the length of a solar day (although it is taken to be 24 hours) is not a constant value. This is due to the fact that the Earth's orbital movement occurs at a variable speed. When the Earth is closer to the Sun, its orbital speed is higher; as it moves away from the sun, the speed decreases. In this regard, such a concept as “average solar day” was introduced, namely its duration is 24 hours.

Orbiting the Sun at a speed of 107,000 km/h

The speed of the Earth's revolution around the Sun is the second main movement of our planet. The Earth moves in an elliptical orbit, i.e. the orbit has the shape of an ellipse. When it is in close proximity to the Earth and falls into its shadow, eclipses occur. The average distance between the Earth and the Sun is approximately 150 million kilometers. Astronomy uses a unit to measure distances within the solar system; it is called the “astronomical unit” (AU).

The speed at which the Earth moves in orbit is approximately 107,000 km/h.
The angle formed by the earth's axis and the plane of the ellipse is approximately 66°33', this is a constant value.

If you observe the Sun from Earth, you get the impression that it is the Sun that moves across the sky throughout the year, passing through the stars and stars that make up the Zodiac. In fact, the Sun also passes through the constellation Ophiuchus, but it does not belong to the Zodiac circle.

Since ancient times, people have been interested in why night gives way to day, winter in spring, and summer in autumn. Later, when answers to the first questions were found, scientists began to take a closer look at the Earth as an object, trying to find out at what speed the Earth rotates around the Sun and around its axis.

In contact with

Earth movement

All celestial bodies are in motion, the Earth is no exception. Moreover, it simultaneously undergoes axial movement and movement around the Sun.

To visualize the movement of the Earth, just look at the top, which simultaneously rotates around an axis and quickly moves along the floor. If this movement did not exist, the Earth would not be suitable for life. Thus, our planet, without rotation around its axis, would be constantly turned to the Sun with one side, on which the air temperature would reach +100 degrees, and all the water available in this area would turn into steam. On the other side, the temperature would be constantly below zero and the entire surface of this part would be covered with ice.

Rotation orbit

Rotation around the Sun follows a certain trajectory - an orbit that is established due to the attraction of the Sun and the speed of movement of our planet. If the gravity were several times stronger or the speed was much lower, then the Earth would fall into the Sun. What if the attraction disappeared or greatly decreased, then the planet, driven by its centrifugal force, flew tangentially into space. This would be similar to spinning an object tied to a rope above your head and then suddenly releasing it.

The Earth's trajectory is shaped like an ellipse rather than a perfect circle, and the distance to the star varies throughout the year. In January, the planet approaches the point closest to the star - it is called perihelion - and is 147 million km away from the star. And in July, the Earth moves 152 million km away from the sun, approaching a point called aphelion. The average distance is taken to be 150 million km.

The Earth moves in its orbit from west to east, which corresponds to the “counterclockwise” direction.

It takes the Earth 365 days 5 hours 48 minutes 46 seconds (1 astronomical year) to complete one revolution around the center of the Solar System. But for convenience, a calendar year is usually counted as 365 days, and the remaining time is “accumulated” and adds one day to each leap year.

The orbital distance is 942 million km. Based on calculations, the speed of the Earth is 30 km per second or 107,000 km/h. For people it remains invisible, since all people and objects move the same way in the coordinate system. And yet it is very big. For example, the highest speed of a racing car is 300 km/h, which is 365 times slower than the speed of the Earth rushing along its orbit.

However, the value of 30 km/s is not constant due to the fact that the orbit is an ellipse. The speed of our planet fluctuates somewhat throughout the journey. The greatest difference is achieved when passing the perihelion and aphelion points and is 1 km/s. That is, the accepted speed of 30 km/s is average.

Axial rotation

The earth's axis is a conventional line that can be drawn from the north to the south pole. It passes at an angle of 66°33 relative to the plane of our planet. One revolution occurs in 23 hours 56 minutes and 4 seconds, this time is designated by the sidereal day.

The main result of axial rotation is the change of day and night on the planet. In addition, due to this movement:

• The earth has a shape with oblate poles;
• bodies (river flows, wind) moving in a horizontal plane shift slightly (in the Southern Hemisphere - to the left, in the Northern Hemisphere - to the right).

The speed of axial movement in different areas differs significantly. The highest at the equator is 465 m/s or 1674 km/h, it is called linear. This is the speed, for example, in the capital of Ecuador. In areas north or south of the equator, the rotation speed decreases. For example, in Moscow it is almost 2 times lower. These speeds are called angular, their indicator becomes smaller as they approach the poles. At the poles themselves, the speed is zero, that is, the poles are the only parts of the planet that are without movement relative to the axis.

It is the location of the axis at a certain angle that determines the change of seasons. Being in this position, different areas of the planet receive unequal amounts of heat at different times. If our planet was located strictly vertically relative to the Sun, then there would be no seasons at all, since the northern latitudes illuminated by the luminary during the daytime received the same amount of heat and light as the southern latitudes.

The following factors influence axial rotation:

• seasonal changes (precipitation, atmospheric movement);
• tidal waves against the direction of axial movement.

These factors slow down the planet, as a result of which its speed decreases. The rate of this decrease is very small, only 1 second in 40,000 years; however, over 1 billion years, the day has lengthened from 17 to 24 hours.

The movement of the Earth continues to be studied to this day.. This data helps to compile more accurate star maps, as well as determine the connection of this movement with natural processes on our planet.

An indisputable fact is the relative motion of the Earth - the Sun. But the question is, what is moving around what?

Copernicus explained: “We are sliding in a boat along a calm river, and it seems to us that the boat and we are not moving in it, and the banks are “floating” in the opposite direction, in the same way it only seems to us that the Sun is moving around the Earth. But in fact, the Earth is moving around the Earth. everything in it moves around the Sun and makes a full orbit within a year.”(L1 p.21) When I was rafting down the river, the banks stood still, and I sailed in a boat past the banks. Everything in the world is relative, either I move relative to the shore, or the shore relative to me. However, the truth is that the water of the river flows relative to the banks. “It is true that Copernicus could not provide direct evidence of the rotation of the Earth and its annual revolution around the Sun, since the level of development of science at that time did not allow this, but the ingeniously simple explanation of the visible movement of the Sun and planets convinced of the validity of his theory.”(L2 p.84) We must pay tribute to Copernicus, he managed to convince many.

The main evidence that the Earth revolves around the Sun is a phenomenon called the annual parallax of nearby stars.

"If you move along the basis AB in Fig. 1, it will seem that the object is displaced against the background of more distant objects. This apparent displacement of an object caused by the movement of the observer is called parallax, and the angle at which the basis is visible from an inaccessible object is called parallax. Obviously, the further away the object is (with the same basis), the lower its parallax...
Even the celestial bodies closest to us are at extremely large distances from the Earth. Therefore, to measure their parallactic displacement a very large basis is required.
When an observer moves across the earth’s surface over distances of thousands of kilometers, a noticeable parallactic displacement of the Sun, planets and other bodies of the solar system occurs.”(L3 p.30) " If you went from Moscow to the North Pole and observed the sky along the way, you would very easily notice that the North Star (or the Pole of the World) is rising higher and higher above the horizon. At the North Pole itself, the stars are located completely differently than in the Moscow sky.”(L1)

Surprisingly, the observer has shifted several thousand kilometers in the orbital plane, sees a change in the celestial sphere, and having shifted in the same plane by almost 300 million kilometers in 6 months, the basis has increased almost 100,000 times, and observes the same insignificant changes. Why? The distances from the Earth to the stars are vast and different, so such a movement in the orbital plane would cause significant changes in the position of the stars in the sky. Parallax is good for characterizing the visual relative motion of objects fixed on the Earth, since it is known what moves and what stands, and in space stars can have their own orbits. Parallax is what it seems to you, so it is not a reliable estimate of what is happening in space. And the ecliptic can be observed both when the Earth rotates around the Sun, and when the Sun rotates around the Earth.

Let me give you an example of relative motion. There are two trains. You are in one of them. Seeing the window, one of them began to move. Which? You look out the window, look at the ground, and it becomes clear to you which train is moving, since you have another point of relative movement, by which you can judge the relative movement of the trains. There is no such point in space between the Earth and the Sun.

Since, from the above, doubts arose about the correctness of Copernicus’s assumption, to determine what revolves around what, I used reliable facts of measuring the daily time of the Earth’s rotation around its axis using the stars and the Sun.

“The simplest time counting system is called sidereal time. It is based on the rotation of the Earth around its axis, which can be considered uniform, since the detected deviations from uniform rotation do not allow 0.005 seconds per day ”(L2 p.46). The daily time according to the stars is 23 hours 56 minutes 4 seconds. "…

To measure Time, the average solar day began to be used, and since the average Sun is fictitious point, its position in the sky calculated theoretically, based on many years of observations of the true Sun.

The difference between mean and true solar Time is called the equation of time. Four times a year the equation of time is zero, and its maximum and minimum values ​​are approximately +15 min" (L4) Fig.2. " The largest discrepancies occur on February 12 (η = +14 m 17 s) and November 3 – 4 (η = -16 m 24 s)"(L2 p52) .

Rice. 2 . Equation of time

Equation of time - the difference between the time shown by a regular clock and the time shown by a sundial.

" The equation of time changes throughout the year in such a way that it is almost exactly the same from one year to the next. Apparent time, and the sundial, can be ahead (fast) by as much as 16 minutes33 sec(around November 3), or behind (slowly) for as much as 14 minutes 6 seconds (around February 12).'' (L5)

‘’ The connection between both solar time systems is established through the equation of time (ŋ), which is the difference between mean time and solar time

ŋ =T λ - T ¤ (3.8) ‘’ (L2 p.52)

Therefore, to determine the true solar time of day when calculating, I add the time from the time equation for a given day to the average solar time. Just as it is said in the textbook and follows from the definition of the equation of time.

The average day according to the Sun contains 24 hours ( L2 Page 51). Therefore, observer H2 (Fig. 4) on February 12 will record a complete revolution around the Sun in 24 hours 14 minutes 17 seconds.3 - 4 November, observer H2 will determine the daily time from the Sun 24h16m24s = 23 hours 43 minutes 36 seconds.
I suggest for comparative analysis place two observers on the equator, the distance between them is 180 0. They measure daily time simultaneously.

Perhaps it is worth noting here that the Earth is akin to a wheel. The rim is the equator, the axis is the imaginary axis of the Earth. To understand why I placed observers at the equator at a distance of 180 0, considermeasuring the time of a rotating wheel (Fig. 3).

On the diameter of the wheel there are time sensors T1 - measuring the rotation time of the wheel according to the light bulb L1 and T2 - by light bulb L2. With uniform rotation, both sensors should show the same wheel rotation time. But if we assume that sensor T1 shows the time of each revolution with an accuracy of 0.005 seconds, and T2 each time shows a time different from T1. The question arises, why? Is the T2 sensor faulty or poorly secured? Or does L2 move? If the sensor is working and well secured, then L2 is moving.

Fig.3

In Fig.4. The star, the Earth, the Sun and observers at the beginning of the daily time count are on the same straight line ZD . H1 measures daily time by the star, H2 by the Sun.
Fig.4

If Copernicus' theory is correct, theno Due to the Earth's orbital motion, H1 will be the first to determine the daily time, and H2 will always be the second. Confirmation of this L2 p.50. “After the sidereal day, the Earth will rotate 360 ​​0 and move along its orbit by an angle of ≈1 0.

In order for...true noon to come again, the Earth needs to rotate another angle of ≈1 0, which will require about 4 m. Thus, the duration of a true solar day corresponds to the rotation of the Earth by approximately 361 0. " Since the distance to the stars is considered unimaginably large, we will assume that∠ O"ZO (Fig. 4) tends to zero, Otherwise there is no way to explain why the stars make a 360 rotation 0 . According to the Earth's orbital motion, it should be smaller. It should be noted that the Earth will make a full revolution when the straight line on which the observers are located becomes parallel to the straight line ZD, since by the beginning of the countdown, observers H1 and H2 are on the straight line ZD. Therefore, observer H1, we will assume, will move to the point “A” will mark the time of the Earth’s complete revolution around its axis relative to the star. Observer H2 will be at point "B". In order for H2 to record the daily time according to the Sun, the Earth must turn to∠BO "D (Fig.4). Once AB is parallel ZD then ∠ BO " D = ∠ O "DO. In other words,the angular distance of the Earth's orbital movement in 23 hours 56 minutes 4 seconds is exactly the angle through which the Earth must rotate for H2 to complete the measurement of daily time according to the Sun.

To answer the question of what revolves around what, I used the theorem: If two parallel lines are intersected by a third line, then the intersecting interior angles are equal.

To overcome ∠ VO" D (Fig.4) February 12 will take time 24h14m17s – 23h56m4s = 18m13s. What corresponds to the rotation of the Earth by an angle 18m13s / 4m ≈ 4.5O. This means that on this day the Earth moves in orbit at an angle of 4.5 o? Or slows down the speed of rotation around its axis for the period of overcoming∠ VO" D , because according to the theory, the Earth cannot travel in orbit more than ≈1 o per day. November 3-4 will spend 12 minutes. 28sec. time is less than H1 according to the stars. For this to happen, the Earth would first have to move in orbit in the opposite direction. It is impossible to simulate the rotation of the Earth around the Sun, according to the equation of time, without changing the direction of motion in orbit and the speed of rotation of the Earth around its axis, since such changes in the Earth’s movement are unnoticed.

In Fig. 5, since during the year the accuracy of measuring the daily time by stars does not exceed 0.005 seconds, for a comparative analysis the method of graphically superimposing three pronounced results of the daily time on each other, obtained by simultaneously measuring the daily time by the stars and the Sun, was used.

H1 – H2 are the positions of daily time observers according to the stars and the Sun, respectively.

D 1 – the position of the Sun, the equation of time is zero, ŋ=0

C, A, B - the position of observer H2 on these days at the end of the measurement of daily time by the Sun.

Fig.5

Earth, Star Z, Sun D and H1, H2 at the beginning of the countdown are on the same straight line ZD . In all cases, the beginning and end of the measurement of daily time by the stars, when the Earth makes a revolution of 360 0, are on the same straight line ZD. As you can see (Fig. 5), the Sun relative to the Earth changes its direction of movement, which is confirmed by the equation of time (Fig. 2).

The main thing in Copernicus' theory is that the Sun is motionless and the Earth revolves around it. This statement is refuted by the facts listed above. The incompatibility of the theory with the obtained results of measuring daily time using the stars and the Sun is obvious. It follows that Ptolemy is right. The Earth does not revolve around the Sun.

The question arises, which model of the relative motion of the Earth-Sun will correspond to the facts listed above, the rotation of the Earth by 360 0 around its axis relative to the stars, the different values ​​of the true day according to the Sun throughout the year. Each of the planets, according to Ptolemy, moves around a certain point. This point, in turn, moves in a circle, in the center of which is the Earth.

Fig.6Fig.7

Let us apply this assumption to simulate the movement of the Sun around the Earth. The rotation of the Sun around the Earth, shown in Fig. 6, removes all the contradictions that arose when considering the theory of the Earth's rotation around the Sun. Dot " W "orbits around the Earth, and around this point" W "The Sun rotates. The Sun moves in orbit around a point" W ", speed relative to the Earth when moving in the direction of the point's orbit " W "increases, and when moving to meet the orbit of the point" W ", decreases and becomes inverse. Therefore, throughout the year, there is a decrease or increase in the true daily time of the Sun relative to the sidereal day.

The sun revolves around the Earth!

Knowing about the change in temperature cycles on Earth, we can assume (Fig. 7) that the Sun rotates around the orbit of point “W” (“barrel”, aerobatics) for 11 years, and the Earth rotates around point “G” in 100 years. At the same time, the Earth changes the inclination of its orbit to the orbit of the point " W ", around which it revolves, over a very long period of time, say 1000 years or more.

Simulator of the rotation of the Sun around the Earth

Direct evidence that the Earth is inside the orbit of the Sun is not only The Equation of Time, but also the Analemma of the Sun. It is worth recalling that:Sine wave- a transcendental flat curved line resulting from double uniform motion of a point - forward and reciprocating in a direction perpendicular to the first.Sine wave - function graphat=sinx, continuous curved line with periodT=2p.

From the point of view of the sinusoidal oscillation of the Equation of Time, the Sun makes two revolutions around the energy point " W " But the orbital movement of the point " W ” and the Sun are carried out in the same direction. Therefore, in fact, the Sun makes three revolutions per year around the point " W " Unfortunately, it is impossible to make a scale model of the movement of the Sun around the Earth. Scale implies maintaining the ratio of sizes, but creating a simulator that explains that the analemma is obtained due to the movement of the Sun in its orbit around the Earth is quite acceptable. Fig. 8 shows such a simulator.

Fig.8

1 - simulator of a small solar orbit.
2 - energy point ‘W’ (aka orbital axis 1).
3 - Sun simulator,
4 - rotation scale of the Sun simulator (graduation in degrees).
5 - tripod.
6 - camera.
7 - tablet on which the camera is mounted.
8 - tripod axis (tilt 23 0 26’).
9 - tripod rotation arrow.
10 - scale of rotation of the tablet and tripod (graduation in degrees).
11 - tablet axis (imaginary axis of the Earth).
12 - base of the simulator.

Since a photograph of the analemma (Fig. 9) is taken after a certain number of days at the same hour of the day, the camera (7) and tripod (5) rotate together. Pictures are taken on the simulator as follows: the tripod is rotated counterclockwise by 10 0, and the small solar orbit simulator (1) is rotated by 30 0. Thus, taking 36 frames per frame, you get an analemma. Of course, not all facts are taken into account here, such as the latitude of the camera and refraction. Yes, this is not necessary. The fact itself is important The analemma is obtained from the rotation of the Sun around the point " W” and dots ‘’ W '' around the Earth.

Fig.9

Afterword

When I accidentally began researching this issue, I discovered that the Earth cannot revolve around the Sun.

I published three articles on the Internet, “Copernicus is great, but truth is more valuable,” “Copernicus’s assumption and reality,” “Ptolemy is right. The sun revolves around the Earth.”In the first article, I tried to determine the distance to the star taken to measure daily time, since the following data is known: sidereal day 23 hours 56 minutes 4 seconds. (86,164sec.); average solar day is 24 hours (86,400 seconds); the radius of the Earth at the equator is 6378160 m; the average speed of the Earth in orbit is 29.8 km/sec. (29,800 m/sec.); linear speed at the equator is 465m/sec. I assumed that the error would be negligible if I neglected the curvature of the Earth and orbit. The calculation amazed me. It turned out that the distance to the star taken to measure daily time is the same as to the Sun and cannot be different. I wrote to the Institute of Astronomy. They answered, read textbooks on Astronomy and that there is a phenomenon of parallax, which is evidence of the rotation of the Earth around the Sun. I started reading. Excerpts that seem to be ignored and which caused me to doubt the correctness of the Copernican theory,is in the second article and in this one. The question arose: is it even possible to determine who is right? Copernicus or Ptolemy. Ptolemy was mistaken in believing that the Earth is the center of the universe, but the center of the solar system is quite acceptable.

In the second article I proved that the Earth rotates according to the stars360 0 . but one of the proofs that the Earth cannot rotate around the Sun was the article by L.I. Alikhanov, which states that the reflected laser signal from a reflector located on the Moon cannot return to the place from which it was sent. Unfortunately it can. You just need to introduce a correction by installing a reflector. In the same article I provided a graph‘’ Equations of time’’ . The graph surprised me by its similarity to sinusoidal oscillations, reflecting movement in a circle. Wrote a letter to the Academy of Sciences. An answer came from the same institute under the same number, although the years were different. I understand them. There are many who want to refute theories and laws, so they imprisoned an employee, and he rivets answers on behalf of the INASAN expert group, so why bother? Maybe they are right. We're flying into space. Well, it turned out that the distance to the stars is 20-25 thousand times closer, but still far away, which makes no one hot or cold. Although, knowing what revolves around what and how, you can make weather forecasts for more than one year.

Lovers of the search for truth, in their free time from work, have one advantage, which is also their disadvantage: they are not burdened with knowledge. But therefore they can make extraordinary assumptions, which should not be brushed aside like annoying flies. We need to figure out what they are right or wrong about. Professionals are often prevented from delving into the works of amateurs due to the conviction that encyclopedic authorities are right. But nothing lasts forever. Theories do not last forever.

The only reliable evidence of what it revolves around can, at the moment, only be Equation of time And Analemma of the Sun, which became the main evidence in this article.

Everything in the world is relative. However, no one would think of saying that the Earth moves relative to the Moon. The Moon moves relative to the Earth against the background of stars. The Sun also moves along the ecliptic against the background of stars. However, the small gravitates toward the big, so it is believed that the Earth rotates around the Sun, but measurements of daily time from the stars and the Sun indicate the opposite.I believe that the Earth is close to a point of increased gravity, so its orbit is inside the orbit of the Sun.

Take a magnet, bring a nail to it, and without even touching the magnet, the nail will begin to have the properties of a magnet. I assume that the universe is something like a collection of gravitational fields (galaxies are flat). Planets and stars being in this field, under its influence, acquire their own gravity, depending on their physical properties. The fields have quiet zones and points with concentrated gravity. The planets of the solar system rotate around such a gravitational charge. I wrote this assumption because I think it explains why the Sun revolves around the Earth.

To answer the question posed to yourself, why is daily time stable according to the stars, but not according to the Sun? I think I managed to answer. - The sun revolves around the Earth.

S.K. Kudryavtsev

Like all the planets of our vast solar system, the Earth makes two main revolutions - around its axis and around the Sun. The time it takes for one rotation of the Earth around its axis is called a day, and the period during which it circles its orbit around the Sun is called a year. This movement is the key to life and physical laws on the planet, according to which we all exist. At the slightest failure (which has not happened yet), the work of all spheres of the Earth, ecosystems and living organisms will be disrupted.

Features of the planet's rotation

Both in the people and in science, the time of one rotation of the Earth around its axis is called a day. They consist of day and night, which last on average 24 hours. Our planet rotates counterclockwise, that is, from west to east. It is thanks to this that residents of the eastern regions are the first to greet the dawn, and the inhabitants of the western hemisphere are the last. An axis is a conventional line that passes through the south and north poles of the planet. Thus, these extreme points do not participate in the rotation process, while all other parts of the earth move.

Since the planet moves from west to east, we can observe how the entire celestial sphere seems to pass by us in the opposite direction, that is, from east to west. This applies to both the Sun and all the stars that we have. The exception is the Moon, since it is an earthly satellite that has an individual orbit.

The movement of our planet in numbers

It is the daily period that determines the speed around the axis. In 24 hours, this celestial body must complete its revolution, taking into account its own parameters and mass. We have already said that the axis permeates the Earth from north to south, and during this process the poles do not rotate around it. At this time, all other zones, including the circumpolar and equatorial ones, move at a certain pace. The speed of rotation of the Earth near the equator is maximum. It reaches 1670 km/h. Moreover, in this area, day and night have an equal number of hours throughout the year.

The Earth's rotation speed in Italy reaches an average of 1200 km/h with a seasonal change in the length of day and night. Thus, the closer we move to the poles, the slower the planet rotates there, gradually coming to zero.

What types of days are there and how are they calculated?

The time of one rotation of the Earth around its axis is called a day, and exactly 24 hours are placed in this interval. But it is worth remembering that there are such concepts as solar days and sidereal days, which have a small but significant difference.

First, let's look at all the features of the first type. Firstly, not every day lasts exactly 24 hours. At those moments when the planet approaches the Sun, its speed of rotation around its axis increases. During periods of distance from the main body of the system, the movement of planet Earth slows down. Therefore, in summer the days may pass a little faster, and in winter they last longer.

As for the sidereal day, its duration is 23 hours, 56 minutes and 4 seconds. This is the time during which our planet rotates around its axis relative to some distant star. That is, if the distant luminary turned out to be the Sun, then the entire rotation, consisting of 360 degrees, would be complete during this period. Well, in order for it to reach the end relative to the Sun itself, it is necessary to go one more degree, which takes just four minutes.

The second important rotation of the planet is around the Sun

The Earth circles the Sun in an elliptical orbit. That is, its circulation occurs not in a clear circle shape, but in an oval pattern. The speed of the Earth around the Sun is on average 107,000 km/h, but this unit is not constant. The average distance of our planet from the sun is 150 million kilometers. An accurate and unchangeable unit is the degree of inclination of the earth's axis relative to the orbit - 66 degrees and 33 seconds, regardless of the time of day or year. It is this inclination, coupled with the shape of the orbit, the variable speed of movement and circulation, that gives us the opportunity to feel seasonal climate changes, but not in all latitudes. If daily fluctuations in time and any changes are multiplied by zero near the poles, then seasonal features also freeze at the equator. Every day from year to year here passes the same way as the previous one, with the same weather, as well as the length of day and night.

The ecliptic and its annual cycle

The term “ecliptic” means a section of the celestial sphere that is within the limits of the Moon. Within the boundaries of this conventional circle, all the main movements of our planet occur, as well as the revolution of the Moon around it. It is worth noting that the latter has a significant influence on the climate, the hydrosphere, and the Moon can be the cause of eclipses, lithospheric metamorphoses and much more.

As for the ecliptic itself, this plane has its own celestial equator, which has certain astronomical coordinates. The inclination of all planets in the solar system is calculated relative to them. The position of the stars and galaxies that we see in the sky is calculated in a similar way (after all, their light falls on the ecliptic, therefore, all those viewed are part of it). This theory is the basis of astrology. According to this science, those constellations that pass through the ecliptic make up the Zodiac. The only unit that does not fall into this category is Ophiuchus. This constellation is visible in the sky, but it is not in the astrological tables.

Summarizing

We have determined that the time of one revolution of the Earth around its axis is called a day. The latter are solar (24 hours) or sidereal (23 hours 56 minutes). The change of day and night occurs in all latitudes of the planet with the exception of the poles. There the earth's rotation speed is zero. The planet's revolution around the Sun occurs every year - 365 days. During this period, there is a change of seasons in all corners of the Earth, but not at the equator. This zone is the most stable, while it rotates around its axis with