How does the aging and dying process of a big star differ from that of the Sun?

Their main-sequence phase is shorter, while the red giant phase is longer.

After the explosion of a large star supernova, a star with a mass of 5 20 times the mass of the Sun will collapse into a neutron star with a diameter of about 10 km, and a mass larger than 20 times the mass of the Sun will collapse into a black hole.

Stars with masses similar to the Sun usually become white dwarfs at the end of their evolution.

The final outcome of a star's evolution depends entirely on its mass.

Stars with masses less than times the mass of the Sun are so small that they will not react with helium after the central hydrogen feedstock is depleted, and can only gradually dim in the form of red dwarfs.

Stars with masses of times to times the mass of the sun will expand and become larger in the later stage of evolution due to the accumulation of helium in the center and the gradual outward movement of the hydrogen fusion reaction region, and the core shrinks after the intensity of the hydrogen fusion reaction decreases, and the reaction of helium fusion into carbon is produced due to the increase of core density and temperature, and new energy is generated. Such an object in the form of a kernel is a white dwarf.

For stars with masses greater than times the mass of the Sun, the inner core will continue to shrink after the reaction of helium fusion to carbon, and carbon fusion will occur into oxygen, neon, magnesium, and sodium. ...and a series of reactions, which will eventually form iron. Then because iron cannot continue to fuse, a supernova explosion occurs, throwing away its gas shell at a very fast rate, eventually becoming a neutron star or black hole.

Stars, like other visible objects in their universe, have a definite life cycle. Stars are born in clouds of gas and dust, and they survive in their own way, eventually dying. This law applies to every star we know, regardless of volume or mass.

Some very large stars have died catastrophically large, and we call this kind of ** "supernova."

Someone sighed. This shouldn't be the star's fate, it should have a milder ending.

We all know that stars have long and short lifespans, so what do these stars become when they age?

A red dwarf, the longest-lived star of the stars, is almost the smallest of the stars, and it becomes a black dwarf when it ages, and the black dwarf is a small ball that does not emit light at all. He will slowly disappear in the universe.

Like the Sun, Sirius.

This type of star, basically, will become a small white ball after **, which will emit a faint bright light, which is a white dwarf.

It's about the size of the Earth.

A star 10 times larger than the Sun** will become a small black ball, denser than a white dwarf, but not a black dwarf, it is a neutron star. It rotates at a speed of 1,000 revolutions per second.

After a star 30 times larger than the Sun**, the planet is about the same size as a neutron star, but the magnetic field is very strong, the planet is called a magnetar, and it can suck iron from your blood from 1,000 kilometers away. But these are not the scariest after the stars.

A star 100 times larger than the Sun** will become a bottomless pit, it will be a black hole, it will suck everything, not even light can escape, if humans get close to it, it will be pulled into spaghetti.

If we were on a planet** dozens of light-years away, it would not be possible for humans to live underground. So what is this thing? The answer is two rays of light from a star.

It's a gamma-ray burst.

Gamma-ray blasts span half the universe. If we were in the Milky Way.

Outside, we can see clearly. There was a gamma burst of gamma rays coming at us. It's bigger than the entire galaxy.

Also, in the American laboratory, they want to imitate the stars**. But they couldn't find a burst of energy that could cause the stellar gamma rays to erupt. In fact, before the star exploded, it was so hot that it made neutrins, and in fact, if you can see neutrins, you can see them everywhere.

There are different types of stars, among which low-mass stars run out of fuel and become red dwarfs as they age; As intermediate-mass stars age, their cores gradually cool down and become small, dense white dwarfs, releasing the remaining energy over a long period of time, gradually dimming, and eventually the white dwarfs that have released their energy become black dwarfs. When the mass is constantly aging, the core will collapse.

Not only stars have lifespans, but planets and a wide variety of other materials do. In the case of the sun, we think of the time that the sun continues to "burn" as its lifespan, and when it stops burning, its lifespan ends.

First of all, it is necessary to explain why the sun "burns". Strictly speaking, the sun is not burning in the mountains, but in nuclear fusion, starting from the core, the hydrogen nuclei fuse into the more massive helium nuclei. So when the fusion is over, the sun is "dead".

Because hydrogen "burns" quickly, according to scientific calculations, the sun has enough hydrogen to "burn" for 10 billion years. The current sun has been "burning" for 5 billion years, which means that the sun is 5 billion years old, just like a person who can live for a hundred years, just over half a hundred, so don't worry, the sun is now in the prime of life.

Comparing hydrogen nuclei and helium nuclei, it can be clearly seen that only 4 hydrogen nuclei can form 1 helium nucleus.

When a star comes out of its "prime", its core will continue to shrink inward, the temperature will become higher and higher, and the burning shell will expand outward, the temperature will gradually decrease, the light emitted will become more and more reddish, and the outer layer will even expand nearly 1 billion times, becoming a huge red giant, and the star will enter its old age.

Stars have a relatively short aging period, and helium fusion ignites when the central compression warms by more than 100 million degrees Celsius. Helium fusion is the fusion of 3 helium nuclei into 1 carbon nucleus, so the main component of the star turns from helium to carbon, and finally forms a small size, large mass, and extremely dense gold ruler in the center, which is like a corrugator, which we call a white dwarf. White dwarfs are small in size, but they are very dense, and a white dwarf the size of a sugar cube weighs 10 tons!

The Sun also becomes a white dwarf when it dies, but if it is a supermassive star (with 30 solar masses), a supernova will eventually occur, forming a mysterious black hole.

Supermassive stars eventually turn into black holes.

The above content refers to Milley's children's book "A Brief History of Life".

Of course! After the fuel of the star is exhausted, it will collapse layer by layer, until it becomes a celestial body with a super density and super super width, and then **, and some will form a super-silver buried nova. Some even form black holes.

Massive stars are stars that exceed the mass of the Sun by more than 7 or 8 times.

The evolution of massive stars from birth to the main sequence stage is similar to that of the Sun, but the later stages of evolution are significantly different.

Due to their huge mass, massive stars expand in the later stages of evolution and are much larger than the Sun, and are called "red supergiants". Some red supergiants are as large as Jupiter's orbital diameter. Sun-mass stars, on the other hand, expand to form red giants, which are much smaller in diameter and volume than red supergiants.

This is the difference between the two in the aging process.

The expansion of a Sun-mass star behind the red giant is a slow stripped of its outer gas in the form of a stellar wind, revealing its stellar core, as a hot white dwarf, and gradually cooling into a black dwarf. The process of demise is calm and relatively long.

Massive stars, on the other hand, quickly shed their outer layers of gas in the form of supernova explosions. This process is very fast, usually only a few days to a few months (in fact, the real burst period is only a few to ten hours), and at the same time, a huge amount of energy is released, and the intensity of the process is unparalleled. Supernova explosions further compress the inner core of a star, which can form a neutron star or black hole, depending on the mass of the initial star.

Neutron stars are the densest form of matter known to mankind, called neutron states. Neutron stars lose energy due to radiation and eventually become invisible due to cooling. Black holes are theoretically infinitely dense and infinitely small "celestial bodies", and their material composition is unknown.

Because its surface detachment velocity is greater than or equal to the speed of light, it is a strong gravitational source in the universe, and no matter (including light) can leave its surface, as if it is a dark bottomless pit in the universe.

The sun is the source of energy for our galaxy, and without it there is nothing else. So will the sun die one day?

The sun continuously emits energy into space in the form of electromagnetic waves, which is released by the fusion of four hydrogen nuclei into one helium nucleus under high temperature and high pressure conditions. We know that the atomic weight of 1 hydrogen nucleus is, the atomic weight of 1 helium nucleus is, and the mass of 4 hydrogen nuclei should be. When 4 hydrogen nuclei fuse into 1 helium nucleus, a unit of mass is lost, and 1 gram of hydrogen nuclei is fused into a helium nucleus.

This means that solar energy is produced at the cost of consuming mass, and this mass is converted into solar radiation and no longer belongs to the sun. The sun loses about 4 million tons of mass per second, which is simply too small for the huge mass of the sun. In the 5 billion years since the birth of the sun, the sun has consumed only mass, and even in another 5 billion years, it will only consume the mass of the sun.

According to this statistics, the mass of the sun will eventually be consumed one day. <>

By studying the evolution of other stars, scientists speculate that hydrogen fusion reactions on the Sun have been going through billions of years so far, with hydrogen decreasing and helium being produced, a period of the Sun's prime of life. When the sun enters old age, it will become a "red giant". At this stage, the star will gradually expand to more than a billion times its size, and the temperature of the surface will decrease, and the luminosity will increase and become very bright.

Once the red giant is formed, it heads towards the next stage of the star, the white dwarf. When the outer region expands rapidly, the helium nucleus is strongly contracted inward by the reaction force, and the compressed material continues to heat up, and eventually the core temperature will exceed 100 million degrees, igniting helium fusion. The final outcome will be the formation of a white dwarf star in the center.

A white dwarf is a low-luminosity, high-density, high-temperature star. For example, Sirius's companion star (it was the first white dwarf to be discovered) is about the size of the Earth, but the mass is about the same as that of the Sun, and its density is about 10 million tons of cubic meters. Since there is no thermonuclear reaction to provide energy, the temperature of the white dwarf will continue to decrease, and eventually it will stop emitting light and become a "black dwarf", floating in the universe all the time.

Whether the Sun will evolve like other stars is still inconclusive. But scientists believe that billions of years from now, the sun will expand rapidly when it is about to die, and the stars and interstellar matter in the solar system will be "swallowed"; In 5 billion years, the Sun will become a red giant. At that time, some life on Earth will die, the oceans will disappear, and the temperature will be two to three times warmer than it is now.

For humanity, it will undoubtedly be the end of the world. But fortunately, the "end of the world" is still far away. With the increasing progress of human science and technology, it is believed that human beings will be able to find a way to survive for themselves by that time.

The first failed star is larger, the second failed star is cooler, and the third failed star will soon end its life.

Young people are like the sun, shining brightly, trying to exert themselves, but failing are like red giants, emitting a dim light, and I think the universe is very profound.

To put it simply, a young star is one that has entered the protostellar stage but has not yet reached the main sequence, and is able to emit light due to thermonuclear reactions within its core, releasing enormous amounts of energy by fusing hydrogen into helium. Whereas a failed star is called a brown dwarf, located between a planet (such as Jupiter) and a star, with a mass less than times the mass of the Sun, and the internal temperature never becomes high enough to reach the temperature at which thermonuclear fusion begins, so although heavier than a gas giant, it is not enough to be a star.

In the universe, young stars are brighter and can transmit energy than failed stars, while failed stars are silent.

Upstairs is also true, but only corresponds to a part of the stars.

The death of a star is not like the death of life, it is quiet and lonely, and it often bursts out with the brightest brilliance of a lifetime before and after death!

For celestial bodies with a much smaller mass than the Sun, there is no way to initiate helium fusion. After the internal energy is exhausted, the nuclear fusion gradually terminates and cools. That's what happened upstairs. (The thermonuclear fusion of ps hydrogen is 4H-He+).

For celestial bodies of similar mass to the Sun, thermonuclear fusion of helium can be initiated. In a certain period of time, his energy is not less and less, but more and more. Evolution to a certain extent, the thermonuclear fusion of helium inside is initiated.

The surface is pushed out, and the diameter can be expanded to more than 100 times the current size. But the surface temperature is very low, which is the red giant. These stars eject material from the surface when helium fusion ceases in their interior, and the landlord can check M57.

For celestial bodies with more than three times the mass of the Sun, it triggers a sea change in heavier elements. In the supergiant stage, it is larger than the Sun and is called a supergiant. ** After the formation of supernovae, the brightness of a star can be compared to a galaxy!

It then evolved into neutron stars or black holes.