What is Solar Optic Motion? The process of solar apparent motion

1.The apparent motion of the sun is what people perceive as the sun rises in the east and sets in the west.

2.To determine the point of the sun, you need to measure the angle between the sun and the ground level at noon, then find the latitude of your place from the map, and then apply the formula directly. The formula is that the height of the Sun at noon is equal to 90 degrees minus the difference between the local latitude and the direct point of the Sun.

3.The date is a bit tricky to calculate, but it can be approximated

The Sun can move north (south) every day and is on the equator on March 21 (September 23). This allows us to rewind the date based on the distance of the Sun from the equator.

4.The observer's position with the Sun can be measured in terms of angles, such as the angle to the ground level and how many degrees to the east (west).

In the morning, the sun rises above the eastern horizon, reaches its highest position at noon, and sets in the west in the evening. The orbit of the sun is felt as if it had passed through an arc in the sky. This transceleral movement of the sun against the background of the celestial dome is known as the sun's apparent motion on Sunday.

In fact, the sun has the other half of its arc orbit below the horizon, but we can't see it. At night, we can also see that all the stars also have this phenomenon of apparent movement in the east and setting in the west.

The movement of the sun in the event horizon. That is, the movement of the sun as seen by the human eye.

Time and space are different, and the angle of the sun's altitude changes from moment to moment. The projection of the sun's apparent trajectory in the celestial sphere is also different at the same time. But they all occur on the ecliptic plane of the Earth's orbit, which is irradiated by the sun's rays.

Because the earth's axis is always tilted in the same direction, the revolution and rotation motion are different, resulting in the difference between the apparent motion of the sun in one day and one year.

In a day, the angle between the rising point of the sun and the line connecting with the center of the earth is the angle between the flat number of the morning and dusk circle and the earth's axis. This angle is somewhere in between. On the winter solstice and the summer solstice, the maximum absolute degree is reached, respectively.

The sun's rays are perpendicular to the morning and dusk faces. There are two intersections between the morning and dusk surface and the wiggling lines at each latitude on the spherical surface. The intersection from night to day is the sunrise point, and the intersection from day to night is the sunset point.

When the polar day occurs in the Arctic Circle, the sunrise point coincides with the sunset point of Tuxiang. Degrees and degrees are mutually reciprocated, and the Antarctic Circle enters the polar night.

The process of solar apparent motion is as follows:

When the Sun deviates the farthest from the north and south ends of the sky, it is the moment when it appears at the two vertices above and below the figure 8 curve, corresponding to the summer solstice and winter solstice of each year. This trajectory of the sun is called the "anklemaline", which is the trajectory of the sun in the sky during the year, with the earth as an observation point.

As long as the sun is recorded at a fixed time, azimuth and angle, the "8" shaped path of the sun can be obtained. The trajectory diagram obtained at different recording time points is also different, the "8" obtained by the morning and evening shooting records is lying flat, and the "8" obtained by the noon shooting records is upright.

In fact, this "8" trajectory is not determined by the sun, but by the earth, because while the earth revolves around the sun, it itself is also rotating, and there is a certain tilt in its rotation axis.

The Earth's orbit is not perfectly circular. In a year, the distance between the earth and the sun is near and far, and the speed of the earth's revolution is also fast and slow, the fastest time point is around January 4 every year, and the slowest cavity number rush time point is around July 4.

The sun is not exactly south at noon every day, sometimes it dies early, sometimes it lags behind, and the maximum time difference is 17 minutes. This also determines the width of the "8" character. In addition to the rotation of the earth, there is also a rotation, and its rotation has an angle of inclination of ° relative to the orbit of the revolution, so the position of the sun at noon will also move in the north-south direction, which also determines the length of the figure "8".

If you can observe the sun's figure-8 trajectory during the day, can you also observe the moon's figure-8 trajectory at night? Like the Earth's orbit, the Moon's orbit is not perfectly circular, but elliptical. On average, the moon appears in the same position in the sky at about 51 minutes.

In other words, if the position of the moon is recorded about 51 minutes later each day than the previous day, a similar "8" trajectory graph can be obtained.

1. First determine the direction on the ground plane.

The general ground direction is the direction of "the cross is guessed", that is, "up the north, down the south, left west, right and early east". However, if you come across a map with a graticule or a map with a pointer, the direction on the "cross" coincides with the direction on the map with the graticule or the map with the pointer, because the two are in some respects the same. Therefore, the orientation on the ground plane can be determined first.

2. Determine the direction of the ground according to the direction of the sun.

The Earth is constantly rotating from west to east, so the Sun rises in the east and sets in the west. The direction on the ground can be determined based on the direction in which the sun rises and sets.

3. According to the position of the known direct sun point and the local latitude position, determine the direction of the sun's apparent movement; Or know the position of the noon sun at a certain latitude of different solar terms to determine the direction in the figure.

The position of the sun relative to the background stars in the day can be considered to be constant, and the moon also rotates from west to east, so from the earth, the moon will move slowly eastward on the sky background, and the apparent motion of the moon is faster than that of the sun, the fundamental reason is that the earth's orbital period is much larger than the moon's orbital period.

The rotation of the Moon is equal to the period of revolution (known as tidal locking), so the Moon always faces the Earth on the same side. The Earth's ocean tides arise mainly due to the gravitational pull of the Moon.

Since the tidal force of the earth's oceans is opposite to the direction of the earth's rotation, the earth's rotation is always subjected to an extremely weak force to "brake" the earth's rotation, which has accumulated over a long period of time, and there is ample evidence that the earth's rotation cycle is getting slower and slower, and the time of the day is increasing extremely slowly, about 1 second in a few years.

The annual apparent motion of the Sun is what the reaction is as follows:

11 years. Solar activity is the general term for all the active phenomena in the solar atmosphere. There are mainly sunspots, light spots, spectral spots, flares, solar and coronal transient events, etc.

Caused by electromagnetic processes in the Sun's atmosphere. The time is strong and sometimes weak, and the average type is based on an 11-year cycle. The Sun during periods of intense activity (known as the "Perturbation Sun") radiates large amounts of ultraviolet light, X-rays, particle streams, and intense radio waves, which often cause phenomena such as auroras, magnetic storms, and ionospheric disturbances on Earth.

Solar activity is a general term for a variety of different activity phenomena in local areas of the solar atmosphere. Includes:

1. Sunspots are the basic markers of solar activity.

2. Light spot: The bright tissue that appears at the edge of the sun's photosphere and extends outward to the color sphere is the spectral spot. The light spots generally surround sunspots and have a close relationship with sunspots.

3. Spectral spots: Plaques that are brighter than the surrounding patches on the sun's photosphere.

4. Solar wind: The flow of charged particles formed by the Taisun Yang wind caused the aurora on the earth.

5. Flare: The powerful short-wave radiation emitted will cause rapid changes in the Earth's ionosphere. The impact on humanity is significant. Causing shortwave communication to be interrupted.

6. Sun: During a total solar eclipse, the sun is surrounded by a red ring with a bright red tongue of fire pulsing on it, and this tongue of fire is called a sun.

7. Corona: The corona is the outermost layer of the Sun's atmosphere (its interior is the photosphere and chromosphere), with a thickness of more than several million kilometers. The coronal temperature is 1 million degrees Celsius and the particle number density is 1015 m3.

At high temperatures, atoms such as hydrogen and helium have been ionized into positively charged protons, helium nuclei, and negatively charged free electrons, etc. The corona can only be seen during a total solar eclipse and when a coronagraph is utilized.

8. Impact: Solar activity is related to volcanic eruptions, droughts, floods, diseases of the human heart and nervous system, and even traffic accidents. Therefore, the science of solar activity forecasting has also been formed.

9. Sunspots are a kind of solar activity that occurs in the photosphere of the sun, and it is the most basic and obvious phenomenon in solar activity. It is actually a huge vortex of hot gas on the surface of the sun, like a shallow disk with a concave middle, and the temperature is 1000 to 2000 times lower than the surface of the photosphere, so it looks "dark".

Be. All the celestial bodies in the universe are moving, and so is the sun. The Sun carries all the large and small bodies of the Solar System, including the Earth, and orbits the center of the Milky Way at a speed of 200 kilometers per second.

Because the galaxy is so large, it takes 200 million years for the sun to orbit around the center of the galaxy. <

Be. All the celestial bodies in the universe are moving, and so is the sun. The Sun carries all the large and small celestial bodies of the Solar System, including the Earth, around the center of the Milky Way at a pre-macro velocity of 200 kilometers per second.

Because the Milky Way is so large, it takes 200 million years for the Sun to orbit around the center of the Milky Way.

Yes, the Sun, like other celestial bodies, rotates from west to east on its axis, but observations and studies have shown that the speed of rotation is different at different latitudes on the surface of the Sun. At the equator, it takes days for the sun to rotate one week, at latitude 40, and at the poles, it takes about 35 days to rotate for one round. This type of rotation is known as "poor rotation".

The Sun revolves around the center of the Milky Way, and the period of its orbit around the center of the Milky Way is about one year. There may be a huge black hole at the center of the Milky Way, but it is surrounded by stars, so it looks like a "silver plate".