If humans live on the earth, write about how people’s lives will change. Write an essay

In the early morning, when the sun bursts out from the red clouds in the sky, spreading golden light to the earth, a vigorous and upward passion will arise spontaneously. Seeing this world full of life, people cannot help but love and praise the sun, the master of all things that gives us life and strength.

The ancestors of the Chinese nation revered their ancestor Yan Emperor as the sun god. In the 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, letting light shine on the earth and sending warmth to the world. He is a god admired by all people. In astronomy, the symbol "⊙" for the sun is very similar to our hieroglyph "sun", which symbolizes the egg of the universe.

The mass of the sun is equivalent to more than 330,000 times the mass 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 109 times the radius of the earth. Even so, she is just an ordinary star in the universe.

The interior of the sun, from the inside out, is composed of three levels: the nuclear reaction zone, the radiation zone, and the convection zone.

The sun is transmitting light and heat to the earth all the time. With sunlight, plants on the earth can carry out photosynthesis. Most plant leaves are green because they contain chlorophyll. Chlorophyll can only synthesize various substances by using the energy of sunlight. This process is called photosynthesis. It is calculated that the entire world's green plants can produce about 400 million tons of protein, carbohydrates and fats every day. At the same time, they can also release nearly 500 million tons of oxygen into the air, providing sufficient food and water for humans and animals. oxygen.

The energy released by the core of the sun spreads outward, causing the surface temperature of the sun to reach approximately 6000°C, like an ocean composed of high-temperature gases. Most of the solar energy is radiated around in the form of heat and light. The giant "nuclear furnace" of the sun has been "burning" stably for 5 billion years. It is currently in its prime, and it will take another 5 billion years before it burns out its nuclear fuel. At that time, it may expand into a huge The red star...

Observing the sun through a general optical telescope, what is observed is the activity of the photosphere (the innermost layer of the solar atmosphere). Many black spots, called sunspots, can often be seen on the photosphere. The size, number, location and shape of sunspots on the sun's surface vary from day to day. Sunspots are local areas of strong magnetic field formed by the violent movement of matter in the photosphere and are important signs of photospheric activity. Long-term observation of sunspots will reveal that some years there are more sunspots, and some years there are fewer sunspots. Sometimes there are no sunspots on the sun for several days or even dozens of days. Astronomers have long noticed that there is a gap of about 11 years from the year with the most (or least) sunspots to the next year with the most (or least) sunspots. In other words, sunspots have an average activity cycle of 11, which is also the activity cycle of the entire sun. Astronomers call the years with the most sunspots "solar activity peak years" and the years with the least sunspots "solar activity quiet years."

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

The energy of the sun comes from its core. The core temperature of the sun is as high as 15 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 takes place here, and 700 million tons of hydrogen are converted into helium every second. During this process, about five million tons of net energy was released (approximately equivalent to 3860 billion trillion megajoules, 3.86 followed by 26 zeros). The energy produced by fusion is transported outward through convection and radiation processes. It takes millions of years for the energy generated in the core to reach the surface.

The radiation zone is outside the core zone

The gas in this layer is also under high temperature and high pressure (but lower than the core zone). Frequent collisions between particles make the core It takes a long time (millions of years) for the energy generated in the convection zone to pass through this layer and reach the convection zone.

Outside the radiative zone is the convection zone

Energy is transferred much faster in the convection zone than in the radiative zone. A large amount of gas in this layer transports energy outwards in the form of convection. (A bit like boiling water, the heated part rises, and the cooled part falls.) The bubble-like structure produced by convection is the "rice grain organization" we see in the photosphere of the solar atmosphere.

The sun is a hot gas planet that emits its own light and heat. Its surface temperature is about 6000°C, and its core temperature is as high as 15 million°C. The radius of the sun is about 696,000 kilometers, which is about 109 times the 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 is 1.4 grams per cubic centimeter, which is about 1/4 of the density of the earth. The average distance between the sun and our earth is about 150 million kilometers.

The sun is an ordinary star in the Milky Way. It is located on the Orion spiral arm north of the Milky Way. It is about 23,000 to 28,000 light-years away from the center of the Milky Way. It orbits the Milky Way at a speed of 250 kilometers per second. The heart rotates, and it takes about 250 million years to complete one revolution. The sun also rotates, and its period is about 25 days in the equatorial zone on the solar surface and about 35 days in the polar regions.

Through the analysis of the solar spectrum, it is known that the chemical composition of the sun is almost the same as that of the earth, but the proportions are different.

The most abundant element on the sun is hydrogen, followed by helium, carbon, nitrogen, oxygen and various metals.

The structure of the sun is mainly divided from the inside out: the center is the thermonuclear reaction zone, outside the core is the radiative layer, outside the radiative layer is the troposphere, and beyond the troposphere is the solar atmosphere.

It can be deduced from the theory of nuclear physics that the center of the sun is the thermonuclear reaction zone. The central region of the sun occupies 1/4 of the entire solar radius and is approximately more than half of the entire solar mass. This indicates that the density of matter in the central region of the sun is very high. Up to 160 grams per cubic centimeter. Under the attraction of its own strong gravity, the central region of the sun is in a state of high density, high temperature and high pressure. It is the birthplace of the huge energy of the sun.

The energy generated in the central region of the sun is transferred mainly in the form of radiation. Outside the central area of ??the sun is the radiative layer. The range of the radiative layer is from 0.25 solar radii at the top of the thermonuclear central area to 0.86 solar radii. The temperature, density and pressure here all decrease from the inside to the outside. In terms of volume, the radiative layer accounts for most of the entire solar volume.

In addition to radiation, the energy inside the sun spreads outwards through convection processes. That is, from 0.86 solar radii of the sun outward to the bottom of the solar atmosphere, this interval is called the troposphere. The properties of this layer of gas change greatly and are very unstable, forming obvious up-and-down convection motion. This is the outermost layer of the Sun's internal structure. Outside the solar troposphere is the solar atmosphere. The solar atmosphere can be divided into photosphere, chromosphere and corona from the inside out. The dazzling sun we see is the intense visible light emitted by the photosphere in the sun's atmosphere. The photosphere is located outside the troposphere and is the lowest or innermost layer of the solar atmosphere. The thickness of the photosphere is about 500 kilometers. Compared with the solar radius of about 700,000 kilometers, it is like the ratio of human skin to muscles. When we say that the average temperature of the sun is about 6000 degrees Celsius, we are referring to this layer. Beyond the light sphere is the color sphere. Normally, because the Earth's atmosphere scatters the intense light balls, the color balls are submerged in the blue sky. Only during a total solar eclipse can you have the opportunity to directly appreciate the red beauty of the chromatic sphere. The solar chromosphere is a magnetic field-filled plasma layer about 2,500 kilometers thick. Its temperature increases from the inside out, from about 4,500 degrees Celsius in the part connected to the photosphere to tens of thousands of degrees Celsius in the outer layer. Density decreases as height increases. The structure of the entire chromosphere is uneven. Due to the instability of the magnetic field, bursts of activity in the upper atmosphere of the sun often occur, resulting in flares.

The corona is the outermost layer of the sun's atmosphere. The material in the corona is also plasma, its density is lower than that of the chromosphere, and its temperature is inversely higher than that of the chromosphere, reaching millions of degrees Celsius. During a total solar eclipse, the very bright silvery white light seen around the sun is the corona.

A patchy tissue in the solar photosphere that is brighter than its surroundings. When observing it with an astronomical telescope, you can often find that some parts of the photosphere's surface are bright and some are dark. This kind of light and dark spots are formed due to the different temperatures here. The darker spots are called "sunspots" and the brighter spots are called "light spots". Spots often "perform" at the edges of the sun's surface, but rarely appear in the center of the sun's surface. Because the radiation in the central area of ??the sun's surface belongs to the deeper gas layer of the photosphere, and the light at the edge mainly comes from the higher parts of the photosphere, so the light spot is higher than the surface of the sun and can be regarded as a "plateau" on the photosphere. ".

The light spot is also a strong storm on the sun, which astronomers jokingly call a "plateau storm." However, compared with ground storms where dark clouds roll, heavy rain pours, and strong winds blow the grass and grass, the "plateau storm" is much milder in character. The brightness of the light spot is only slightly stronger than the quiet photosphere, generally only 10% larger; the temperature is 300°C higher than the quiet photosphere. Many light spots are closely related to sunspots and often "perform" around sunspots. A small number of spots have nothing to do with sunspots. They are active in the high latitude area of ??70° and have a relatively small area. The average lifespan of the spots is about 15 days, and the lifespan of larger spots can be up to three months.

Light spots not only appear on the photosphere, but also on the chromosphere. When it "performs" on the chromosphere, the location of the activity roughly coincides with when it appears on the photosphere. However, what appears on the chromosphere is not called a "light spot" but a "spectral spot".

In fact, the light spot and the spectrum spot are the same whole, just because their "residences" are at different heights. It is like a building, the light spot lives downstairs, and the spectrum spot lives upstairs.