Diameter: 1.39 million km.
Mass: 1.989e30
Temperature: 5800 K (surface)
15.6 million (core)
The sun is the largest object in the solar system. It has 99.8% of the total mass of the solar system (Jupiter has most of the rest).
The sun is personified in many myths: the ancient Greeks called it the sun god, while the ancient Romans called it the sun god.
The mass of the sun is composed of 75% hydrogen and 25% helium (92. 1% atomic number is hydrogen and 7.8% helium); The total amount of other substances ("metals") is only 0. 1%. At the core of the sun, hydrogen is converted into helium, and these quantities change slowly.
The outer layer of the sun has different rotation periods: the equatorial plane rotates once every 25.4 days; The polar region reached 36 days. This strange phenomenon is because the sun is not a solid sphere like the earth, and a similar situation can be seen on gaseous planets. So in the sun, the rotation period is also different, but the core of the sun still rotates like a solid.
The state of the sun's core is amazing, with the temperature reaching15,600,000 Kelvin and the pressure equivalent to 250 billion atmospheres. The gas in the core is compressed to 150 times the density of water.
The energy released by the sun is 3.86e33 erg/s (3.86 trillion MW), which is produced by nuclear fusion reaction. Every second, about 700,000,000 tons of hydrogen atoms are converted into about 695,000,000 tons of helium atoms, and 5,000,000 tons of energy (= =3.86e33 erg) are released in the form of gamma rays. Because the radiation is emitted to the surface of the sphere, it constantly absorbs and emits energy, which makes the temperature drop continuously, so the temperature difference between inside and outside is huge, and it is basically visible light. The energy output by convection is at least 20% higher than that by radiation divergence.
The outer surface of the sun is called the photosphere, and the temperature is about 5800 K. Sunspots are "cool" places on the sun, only 3800 km (because they look darker than the surrounding areas). Sunspots can be very large, with a diameter of 50 thousand kilometers. Sunspots are produced by the complex and unknown action of the solar magnetic field.
A small area above the photosphere is called chromosphere.
The wide and thin material above chromosphere is called a solar halo, which extends into space for millions of kilometers, but can only be observed during the solar eclipse (left). The internal temperature of the solar flare exceeds 1 1,000,000 K.
The solar magnetic field is extremely powerful (by the standards of the earth) and very complicated. Its magnetosphere is even much larger than Pluto.
In addition to light and heat, the sun also emits low-density particle streams (mostly electrons and protons) to form a solar wind, which propagates in the solar system at a speed of 450 km/s. When the solar wind and high-energy particles shine on the sun, it will have an impact on tidal waves and radio communication on the earth, and will produce aurora.
Recent data from the Ulysses spacecraft show that the speed of solar wind diverging from the poles has doubled to 750 km/s, which also occurs in low latitudes. The composition of the solar wind in the polar regions is also different, and the solar magnetic field seems surprisingly unstable.
More research on the solar Wind will be completed with the help of Wind, ACE and SOHO spacecraft in the near future. They will take advantage of dynamic stability and be located directly between the earth and the sun, 65,438+0,600,000 kilometers away from the earth.
The solar wind causes comets to produce tails, and sometimes even has measurable effects on the orbit of spacecraft.
Spectacular annular protrusions, corona, also often appear at the edge of the sun. (Left)
The energy output of the sun is unstable, and the number of sunspot activities is also unstable. /kloc-there was an unusually weak sunspot activity period in the second half of the 0/7th century, which was consistent with the abnormal low temperature period (Little Ice Age) in northern Europe at that time. Since the formation of the sun, energy output has increased by 40%.
The sun is 4.5 billion years old. Since its birth, it has used half of the hydrogen atoms in its core. It will still radiate "gently" for about 5 billion years (although the brightness will be twice as high as it is now), but it will eventually run out of energy. At that time, it will be in an extremely unstable state, and with the change of state, it will eventually destroy the earth together (possibly forming a brand-new planetary system).
The satellite of the sun
There are nine planets and a large number of other small celestial bodies revolving around the sun. To be exact, there is a debate about the standards of planets and small celestial bodies. In the final analysis, it's just a question of definition.
Planetary Distance (km) Radius (km) Mass (kg) Discoverer Discovery Date
Mercury 57,91000 2439 3.30e23
Venus108,200,000 6052 4.87e24
Earth149,600,000 6378 5.98e24
Mars 227,940,000 3397 6.42e23
Jupiter 778330000 714921.90e27
Saturn 1, 426,940,000 60268 5.69e26
Uranus 2,870,990,000 25559 8.69E25 Herschel 178 1.
Neptune 4,497,070,000 247641.02e26 Galle1846.
Pluto 5,913,520,0001601.31e22tombaugh1930.
Radius of basic physical parameters of the sun: 696,295 km. T6。
Mass: 1.989× 1030kg =u(s
Temperature: 5800℃ (surface) Zy
1560000℃ (core) j*nb
Total radiation power: 3.83× 1026 Joule/sec x.
Average density:1.409g/cm3 3c.
Average distance between the sun and the earth:1.500 million km AP
Age: about 5 billion years 6
Text heaven-home of astronomy enthusiasts-text heaven 2 = l:
For human beings, the brilliant sun is undoubtedly the most important celestial body in the universe. Everything grows on the sun. Without the sun, there would be no various life phenomena on the earth, and of course there would be no human beings as intelligent creatures. The sun gives people light and heat, brings the cycle of day and night and seasons, affects the change of the earth's temperature, and provides various forms of energy for life on earth. A
Text paradise-home of astronomy lovers-text paradise > o
In human history, the sun has always been the object of worship by many people. The ancestors of the Chinese nation regarded their ancestor Yan Di as the sun god. In ancient Greek mythology, the sun god was the son of Zeus (the king of gods). \/
Gobbledygook-home of astronomy lovers-gobbledygook
The sun, an awesome planet, is made of what material and what is its internal structure? "v & VI
Text Paradise-Home of Astronomers-Text Paradise _2HA
In fact, the sun is just a very ordinary star. In the vast star world, the brightness, size and material density of the sun are at a medium level. Because it is closest to the earth, it looks like the biggest and brightest celestial body in the sky. Other stars are far from us. Even the nearest star is 270,000 times farther away from the sun, and looks like flickering light. |] CC @V
Text Paradise-Home of Astronomers-Text Paradise AQKK$
Most of the substances that make up the sun are ordinary gases, of which hydrogen accounts for about 7 1%, helium accounts for about 27% and other elements account for 2%. From the center to the outside, the sun can be divided into nuclear reaction area, radiation zone, convection zone and solar atmosphere. The atmosphere of the sun, like that of the earth, can be divided into three layers according to different heights and different properties, namely, the photosphere, the chromosphere and the corona. The surface of the sun we usually see is the bottom of the sun's atmosphere, and the temperature is about 6000 degrees Celsius. It is opaque, so we can't directly see the internal structure of the sun. However, according to the physical theory and the study of various phenomena on the surface of the sun, astronomers have established a model of the internal structure and physical state of the sun. This model has also been confirmed by the research of other stars, at least in a big way, it is credible. L4f7h^
The Text of Heaven-The Home of Astronomers-The Text of Heaven uuz
Although the core area of the sun is very small, the radius is only 1/4 of the radius of the sun, but it is the real source of the great energy of the sun. The temperature of the sun's core is extremely high, reaching 15 million℃, and the pressure is also extremely high, which makes the thermonuclear reaction of hydrogen fusion into helium occur, thus releasing huge energy. These energies can only be transferred through the matter in the radiation layer and troposphere, transmitted to the bottom of the solar photosphere, and then radiated through the photosphere. @; wXG
The text of heaven-the home of astronomy lovers-the text of heaven Kp
The photosphere of the sun is the round surface of the sun that we usually see, and the radius of the sun usually refers to the radius of the photosphere. The surface of the photosphere is gaseous, and its average density is only several hundred million times that of water, but due to its thickness of 500 kilometers, the photosphere is opaque. There is strong activity in the atmosphere of the photosphere. With a telescope, we can see that there are many dense point structures on the surface of the photosphere, which are very similar to rice grains. They are called rice grain tissues. They are extremely unstable, generally lasting only 5 ~ 10 minutes, and their temperature is 300 ~ 400℃ higher than the average temperature of the photosphere. At present, it is believed that this particle structure is caused by intense convection of gas under the photosphere. \c7^wX
Text paradise-home of astronomy lovers-text paradise l[zQoM]
Another famous activity phenomenon on the surface of the photosphere is sunspots. Sunspots are huge air swirls on the photosphere, most of which are nearly oval, which are darker against the bright photosphere background, but in fact their temperature is as high as 4000℃. If the sunspot can be taken out alone, a large sunspot can emit the light equivalent to a full moon. The appearance of sunspots on the surface of the sun is constantly changing, reflecting the change of solar radiation energy. The change of sunspots has complex periodicity, and the average activity period is 1 1.2 years. Five; n
Text Paradise-Home of Astronomers-Text Paradise 7)O5
The atmosphere near the photosphere is called chromosphere, which is not easy to be observed at ordinary times. In the past, this area was only visible during a total solar eclipse. When the moon hides the bright brilliance of the ball of light, people can find that there is a rosy brilliance on the edge of sun gear, that is, the ball of color. Chromosphere is about 8,000 kilometers thick, and its chemical composition is basically the same as that of the photosphere, but the density and pressure of matter in chromosphere are much lower than that of the photosphere. In daily life, the farther away from the heat source, the lower the temperature, but in the solar atmosphere, the opposite is true. The temperature at the top of the photosphere near chromosphere is almost 4300℃, but it reaches tens of thousands of degrees at the top of chromosphere, and then rises to several million degrees in the corona. People are puzzled by this abnormal warming phenomenon, and the exact reason has not been found so far. {*A
The Text of Heaven-Home of Astronomers-The Text of Heaven z'(~
People can also see many soaring flames on the color ball, which is the so-called "prominence" in astronomy. Prominence is a rapidly changing activity phenomenon, and a complete prominence process usually takes dozens of minutes. At the same time, the shape of prominence can be said to be varied, some like clouds, some like waterfalls and fountains, some like curved arch bridges, some like grass, and the list goes on. Astronomers classify prominences into three types according to the size and speed of morphological changes: quiet prominences, active prominences and explosive prominences. The most spectacular is the explosive prominence, which is quiet or active. Sometimes, it will suddenly become "violent", desperately throwing gas up, and then turning back to the surface of the sun to form a ring, so it is also called an annular prominence. IDF=a
Text paradise-home of astronomy enthusiasts-text paradise uhcoO2
In the brief moment of total solar eclipse, you can often see a large white, blue, soft and beautiful halo around the sun, which is the outermost layer of the solar atmosphere-corona. The corona extends over the chromosphere and extends to several solar radii. The material in the corona is thinner, which will expand outward and make thermoelectric gas particles flow out of the sun continuously, forming the solar wind. k
Text of Heaven-Astronomer's Home-Text of Heaven 4e
The sun looks calm, but in fact it has been moving violently. Active phenomena on the surface of the sun and the atmosphere, such as sunspots, flares and coronal mass ejections, will greatly enhance the solar wind, resulting in many geophysical phenomena, such as the increase of aurora, the changes of atmospheric ionosphere and geomagnetic field. Solar activity and the enhancement of solar wind will also seriously interfere with the normal work of radio communication and space equipment on the earth, damage the precision electronic instruments on satellites, cause chaos in the ground power control network, and even pose a threat to the lives of astronauts in the space shuttle and space station. Therefore, it is becoming more and more important to monitor solar activity and solar wind intensity and make "space weather" forecast in time. & amp'
Textual Heaven-Home of Astronomers-Textual Heaven+1-
Among the 1000 billion stars in the Milky Way, the sun is just an ordinary member. It is located near the symmetry plane of the Milky Way, about 26,000 light years away from the center of the Milky Way and 26 light years north of galactic plane. On the one hand, it rotates around the center of the Milky Way at a speed of 250 kilometers per second, and on the other hand, it moves near Vega at a speed of 19.7 kilometers per second relative to the surrounding stars. 5yk
The sun gives off colorful light. The sun. This is an image of Iron XII with a wavelength of 19.5nm. In the picture, several bright areas are active areas of the sun, several dark areas are coronal holes, and a circle around them is a corona. SOHO shooting. The sun. These four solar images were taken in different elemental spectral lines and different wave bands, among which (a) iron IX/X, 17. 1nm (b) iron XII, 19.5nm (c) iron XV, 28.4nm (d) helium II/ silicon XI, 30.4. Schematic diagram of the internal structure of the sun. f
Sunspots. The umbra and penumbra of sunspots. Flares in sunspot areas. Particle structure of the photosphere of the sun. /e
Corona. SOHO detector shooting. Corona. June 199 1+0 during the total solar eclipse. Corona. 4-inch refracting telescope1February, 1998. Corona. 1August, 998 1 1 taken at the lake Haza in eastern Turkey. ^(h3
Prominence and corona. Taken during the total solar eclipse. Prominence eruption (upper right corner). SOHO shot on1September, 999 14. Prominences erupt (lower right corner). Sun X-ray images from 199 1 year1month after the launch of "Sunshine" to the end of 1995. The solar activity in the picture is very obvious from prosperity to decline. Photographed by the "Sunshine" detector. 1
The sun. SOHO shooting. At sunset. At sunset. 1999 April 16 photo taken in Sicily, Italy. Summer sunshine. Taken in June 1996. Vkq！
The sun is shining. Taken in Laguna Mountain, California, USA. The sun.