The composition of immigrant life on earth

In the morning, when the sun bursts out from the rosy clouds all over the sky, sprinkling golden light on the earth, a vigorous passion will come out of generate. Seeing this vibrant world, people can't help loving and praising the sun, which is the master of all things and gives us life and strength.

The ancestors of the Chinese nation regarded their ancestor Yan Di as the sun god. In colorful Greek mythology, the sun god is called "Apollo". He holds a lyre in his right hand and a golden ball symbolizing the sun in his left hand, which makes the light shine on the earth and sends warmth to the world. He is the god that everyone worships. In astronomy, the symbol "⊙" of the sun is very similar to our hieroglyph "Sun", which symbolizes the egg of the universe.

The mass of the sun is more than 330,000 times that of the earth, its volume is about 1.3 million times that of the earth, and its radius is about 700,000 kilometers, which is more than 1.09 times that of radius of the earth. Even so, she is just an ordinary star in the universe.

The interior of the sun, from the inside out, consists of nuclear reaction area, radiation zone and convection zone.

The sun has been transmitting light and heat to the earth. With sunlight, plants on the earth can carry out photosynthesis. The leaves of most plants are green because they contain chlorophyll. Chlorophyll can only use the energy of sunlight to synthesize various substances. This process is called photosynthesis. According to calculation, green plants all over the world can produce about 400 million tons of protein, carbohydrates and fat every day, and at the same time release nearly 500 million tons of oxygen into the air, providing sufficient food and oxygen for people and animals.

The energy released by the sun's core spreads outward, making the surface temperature of the sun reach about 6000℃, just like an ocean of high-temperature gas. Most of the solar energy radiates to the surroundings in the form of light and heat. The sun, a huge "nuclear melting pot", has been burning steadily for 5 billion years. At present, it is in the prime of life, and it will take another 5 billion years to burn out nuclear fuel. At that time, it may expand into a huge red star. ...

Observing the sun through ordinary optical telescopes, we observe the activities of the photosphere (the innermost layer of the sun's atmosphere). You can often see many black spots on the photosphere, called sunspots. The size, number, location and shape of sunspots on the sun's surface are different every day. Sunspot is a local strong magnetic field formed by the violent movement of photosphere, and it is an important symbol of photosphere activity. Long-term observation of sunspots will show that there are many sunspots in some years, few sunspots in some years, and sometimes there are no sunspots in the sun for several days or dozens of days. Astronomers have long noticed that there is an interval of 1 1 year from the year with the most (or least) sunspots to the next year with the most (or least) sunspots. In other words, the average activity period of sunspots is 1 1, which is also the activity period of the whole sun. Astronomers call the year with the most sunspots "the peak year of solar activity" and the year with the least sunspots "the quiet year of solar activity".

The interior of the sun can be divided into three layers: core region, radiation region and convection region.

The energy of the sun comes from its core. The core temperature of the sun is as high as 654.38+05 million degrees Celsius, and the pressure is equivalent to 250 billion atmospheres. The gas in the core area is extremely compressed to 150 times the density of water. Nuclear fusion is taking place here, and 700 million tons of hydrogen is converted into helium every second. In this process, about 5 million tons of net energy (about 3.86 trillion megajoules, followed by 26 zeros) is released. The energy produced by fusion is transferred by convection and radiation. The energy generated by the core takes millions of years to reach the surface.

The radiation area is wrapped outside the core area.

The gas in this layer is also in a state of high temperature and high pressure (but lower than that in the core region), and the frequent collisions between particles make it take a long time (millions of years) for the energy generated in the core region to pass through this layer and reach the convection region.

Outside the radiation zone is the convection zone.

The energy transfer in convection zone is much faster than that in radiation zone. A large amount of gas in this layer transports energy by convection. It's a bit like boiling water, where the heated part rises and the cooled part falls. The bubble-like structure produced by convection is the "granular structure" we see in the photosphere of the solar atmosphere.

The sun is a hot gas planet, and it glows and heats itself. Its surface temperature is about 6000℃, and its center temperature is as high as150,000℃. The radius of the sun is about 696,000 kilometers, which is about 109 times that of radius of the earth. Its mass is 1.989× 10 27 tons, which is about 332,000 times that of the earth. The average density of the sun is1.4g per cubic centimeter, which is about 1/4 of the density of the earth. The average distance between the sun and the earth is about1.500 million kilometers.

The sun is an ordinary star in the Milky Way, located on the spiral arm of Orion, north of galactic plane, about 230,000 to 28,000 light years away from the center of the Milky Way. It rotates around the center of the Milky Way at a speed of 250 kilometers per second, and it takes about 250 million years to make a revolution. The sun is also rotating, and its cycle is about 25 days in the equatorial belt; The polar region is about 35 days.

Through the analysis of the solar spectrum, we know that the chemical composition of the sun is almost the same as that of the earth, but the ratio is different. The most abundant element in the sun is hydrogen, followed by helium, carbon, nitrogen, oxygen and various metals.

From the inside out, the structure of the sun is mainly divided into: the central thermonuclear reaction zone, the radiation layer outside the core, the troposphere outside the radiation layer and the solar atmosphere outside the troposphere.

Inferred from the theory of nuclear physics, the center of the sun is a thermonuclear reaction zone. The central area of the sun accounts for 1/4 of the entire solar radius, which is about half of the entire solar mass. This shows that the material density in the central region of the sun is very high. It can reach 0/60 grams per cubic centimeter/kloc. The central area of the sun is in a state of high density, high temperature and high pressure under the attraction of its own strong gravity. It is the birthplace of the great energy of the sun.

The energy generated in the central region of the sun is mainly transmitted by radiation. Outside the central area of the sun is the radiation layer, which ranges from 0.25 solar radius at the top of the central area of the thermonuclear to 0.86 solar radius, and the temperature, density and pressure decrease from the inside out. In terms of volume, the radiation layer accounts for the vast majority of the whole solar volume.

In addition to radiation, the energy inside the sun spreads outward, and there is also a convection process. That is, from the solar radius of 0.86 to the bottom of the solar atmosphere, this interval is called the troposphere. The properties of this layer of gas vary greatly and are unstable, forming obvious up-and-down convection movement. This is the outermost layer of the inner structure of the sun. Outside the troposphere is the solar atmosphere. The solar atmosphere can be divided into photosphere, chromosphere and corona layer from inside to outside. What we see is the dazzling sun, which is the intense visible light emitted by the photosphere in the solar atmosphere. The photosphere is located outside the troposphere and belongs to the lowest or innermost layer of the solar atmosphere. The thickness of the photosphere is about 500 kilometers, which is like the ratio of human skin to muscle relative to the radius of the sun of about 700 thousand kilometers. When we say that the average temperature of the sun is about 6000 degrees Celsius, we mean this layer. Beyond the ball of light are colored balls. Usually, due to the strong photosphere scattered by the earth's atmosphere, chromosphere is submerged in the blue sky. Only during the total solar eclipse will you have a chance to directly appreciate the red appearance of the colored ball. The solar chromosphere is a plasma layer full of magnetic field, about 2500 kilometers thick. Its temperature rises gradually from the inside out, the part connected with the top of the photosphere is about 4500 degrees Celsius, and the outer layer reaches tens of thousands of degrees Celsius. The density decreases with the increase of height. The whole structure of chromosphere is uneven. Due to the instability of the magnetic field, the upper atmosphere of the sun often explodes and flares occur.

The corona is the outermost layer of the solar atmosphere. The material in the corona is also plasma, the density is lower than that of chromosphere, and the temperature is higher than that of chromosphere, reaching several million degrees Celsius. During the total solar eclipse, very bright silvery white light can be seen around the surface of the sun, which is the corona.

Spotted tissue on the photosphere of the sun that is brighter than the surrounding area. When observing with an astronomical telescope, it is often found that the surface of the photosphere is bright and dark. This bright and dark spot is formed because of the different temperatures here. The darker points are called "sunspots" and the brighter points are called "sunspots". Sunspots often "perform" on the edge of the sun's surface and rarely appear in the central area of the sun's surface. Because the radiation in the central area of the sun's surface belongs to the deep gas layer of the photosphere, and the light at the edge mainly comes from the higher part of the photosphere, the light spot is higher than the sun's surface and can be regarded as a "plateau" on the photosphere.

Sunspots are also strong storms on the sun, which astronomers call "plateau storms". However, compared with the ground storm with dark clouds rolling and heavy rain and strong winds, the character of "plateau storm" is much gentler. The brightness of the light spot is only slightly stronger than that of the quiet photosphere, generally only10%; The temperature is 300℃ higher than that of the quiet photosphere. Many sunspots have an indissoluble bond with sunspots, and they often "perform" around sunspots. A small number of sunspots have nothing to do with sunspots, and are active in the 70 high latitude area, with a relatively small area. The average life span of spots is about 15 days, and the life span of larger spots can reach three months.

The light spot not only appears in the photosphere, but also has its activity place in chromosphere. When it "performs" on the color ball, the position of the activity is roughly the same as when it appears on the light ball. However, what appears on the color ball is not a "light spot", but a "spectral light spot". In fact, the light spot and the spectral spot are the same whole, just because their "resident" heights are different. It's like a building, where the light spot lives downstairs and the spectrum spot lives upstairs.