Why do big stars die very often?

The vast majority of the stars we see in the night sky are stars, and they are generated at different times, the "old" ones are more than 10 billion years old, and the "new" stars may only be hundreds of millions of years old; And the size of the stars is also very different, and it can vary by tens or even thousands of times.

The "big stars" you are talking about will soon "die", and the "big stars" here should generally refer to the stars that are already in the "old age", they have been burned and consumed for tens of billions of years or even longer, and their own mass is only tens of thousands or even millions of times when they were "young", and the interior of the star has been empty, resulting in a serious collapse, for the final combustion and eruption, they use more energy to maintain, and the collapse has produced a great reaction force, Therefore, the volume of such stars will appear very large, hundreds or thousands of times larger, but their surface temperature is generally about 3,000 degrees Celsius, which is half or even only a fraction of the original. The light of these stars is now very dim, and it is no longer as bright and dazzling as it used to be, and they are distinctly red when viewed from Earth. Therefore, astronomy refers to such stars as "red giants".

For these reasons, the red giant does not have much time to last, and in the end, it will use the last bit of "power" left to "shine back", and the final total explosion will occur, at which point it is one of the brightest stars in the universe, and they are called "supernovae".

The material from supernovae can travel far, even several light-years. After a while, this material will slowly coalesce with other interstellar wandering matter and re-condense into a sizable star, at which point it will be reborn!

This is what you call a big star that will "die" very quickly!

Large stars need greater outward force to maintain themselves because of their greater "gravity", so they consume fuel much faster than small stars.

Overall, large stars will have shorter lifespans than smaller stars.

Betelgeuse; two stars of the sea and seamount of the ship's base; Horn Decienda (Virgo star); Pegasus ik.

Under Earth's ideal conditions, about 9,000 stars can be seen with the naked eye. The nearest is the star Centauri, which is light-years away. The most distant is Cassiopeia V762, which is about 16,000 light-years away.

The vast majority of existing stars are lower-massive, longer-lived stars, but the brightest and easiest to see are giants and supergiants.

Giants are a class of late stars that die out shortly after evolving into supernovae or planetary nebulae. Supergiants are the shortest-lived stars, with a total lifespan of less than 10 million years.

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Stars are giant spheres made of light-emitting plasma, mainly hydrogen, helium, and trace amounts of heavier elements. On a clear night, there are countless points of light in the night, and most of them are stars except for a few planets.

The Sun is the closest star to Earth, and almost all of the stars that can be seen at night are in the Milky Way. Of the approximately 300 billion stars in the Milky Way system, only a fraction of them can be observed.

Stars undergo nuclear fusion at their cores to produce energy that is transmitted outward, then radiated from the surface into outer space. Once the nuclear reaction in the core is exhausted, the life of the star is coming to an end.

At the end of life, stars also contain degenerate matter. Differences in the size and mass of stars lead to different outcomes: white dwarfs, neutron stars, black holes.

When a star dies, it eventually becomes one of three things: a white dwarf, a neutron star, and a black hole.

If you want to become a white dwarf after death, the star must be a small and medium-sized star, and in the process of death, two parts are formed, the star shell and the star core, the star shell is ejected outward, the star core collapses inward, and if the mass of the star core is not greater than the mass of the sun, a white dwarf will be formed. When a white dwarf is under high pressure, the atoms are crushed, and the electrons will deorbit and become free electrons.

In general, the mass of such a star before death is about 8 to 10 times the mass of the Sun. According to theoretical speculation, white dwarfs make up about 10% of the total number of stars.

If a star wants to become a neutron star, then its mass must be more than 8 10 times the mass of the sun, and less than 30 times, so as to ensure that the star will have a supernova when it dies, and the mass of the inner core will remain between times the mass of the sun, and finally under high pressure, not only the atoms will be crushed, but the nucleus will also be crushed, and the protons and electrons will combine to form neutrons, and finally, all the neutrons will be compressed together to form a neutron star.

Stars that are twice as massive as the Sun die and become neutron stars, more than twice as massive as the Sun become black holes, and those smaller than the Sun become white dwarfs (including the Sun).

As the megamolecular cloud orbits a galaxy, events may cause its gravitational collapse to collapse. Macromolecular clouds may collide with each other or pass through dense parts of the spiral arms. The high-velocity mass thrown by a nearby supernova explosion is also a trigger.

Finally, nebulae compression and perturbations caused by galaxial collisions may also form a large number of stars.

Those that are twice as massive as the Sun die and become neutron stars, those that are more than twice as massive as the Sun become black holes, and those smaller than the Sun become white dwarfs.

The evolution of stars can be roughly divided into the following stages:

1. The main sequence is the previous stage, and the star is in its infancy.

2. The main sequence is the star stage, and the stars are in their prime.

3. In the red giant stage, the star is in middle age.

4. In the white dwarf stage, the star is in old age. Most stars spend their lives in this way.

A star is a spherical luminous plasma held together by gravity, and the Sun is the closest star to Earth.

Almost all of the other stars that can be seen on Earth at night are within the Milky Way, but due to their distance, these stars appear to be just fixed points of light. Historically, the more prominent stars have been grouped into constellations and constellations, with the brightest stars having their own traditional names.

Less than a solar mass will evolve into a white dwarf, and a solar mass will evolve into a neutron star. Twice the mass of the Sun is a black hole.

First of all, every star dies, but it is impossible for a planet to become a nebula, a white dwarf, or a black hole, and these consequences are only endured by a celestial body that can shine on itself, and the planet is not capable of becoming some.

Take the Earth as an example, the Earth is a planet, and she may have some endings:1Perished by the impact of alien bodies.

2.In the late sun, it swallowed the earth and caused it to perish.

3. There are also some human factors, etc.

However, nebulae, white dwarfs, and black holes are the home of stars.

Take the sun as an example, the sun will eventually become a white dwarf, followed by a black dwarf, which will not emit light, and there will be some material around the sun that has exploded before, and in the middle is a white dwarf, which is called a planetary nebula.

Black holes need to be more than 8 to 12 times the mass of the Sun to form, which means that when a planet dies, it may become cosmic dust.

Hope it helps.

The life cycle of galaxies is not as well-defined as that of stars. Scientists used to believe that all galaxies formed on their own in a relatively short period of time, but the process of formation of the Milky Way proves that this idea is almost false.

Does a star like the Sun die? I've lived for an unknown number of years.

When a super-large star dies at the end of its life, it undergoes hydrogen-helium fusion and becomes a supernova. At the end of a star's life, we call it a supernova. Let's start by looking at stars, which come in all colors, shapes, and sizes, like blue giants, red giants, superred giants, and our sun is a yellow dwarf.

Despite these differences, most of them end their lives as supernovae. The question is, what is a supernova? Supernovae are large-scale splits that occur at the end of a star's life cycle, so the question is what causes supernovae?

Supernovae occur when the core or center of a star changes. This change can occur in two different forms, both of which lead to supernovae. Let's take a look at the types of superstars that occur in binary star systems.

A binary star system consists of two stars orbiting a common center, and in the process, one of the constancy is a white dwarf that takes material from its partner star. Eventually, the white dwarf accumulates too much material, but it can't digest it, causing the star** to become a supernova. Another type of supernova occurs at the end of a single star's lifespan, when the star runs out of fuel and some of its material flows into the core.

Eventually, the mid-star part of the star is too heavy to withstand its own gravity and becomes like a time bomb. Finally the core collapsed, all the matter and radiation was gone, which led to a terrible explosion, which we call supernovae, not all stars have ended up supernova, just like our sun is also a star, but it does not have enough mass to be a supernova, otherwise it will pose a major threat to the planets in our solar system. Do you know?

Although a supernova only occurs for a short period of time, it can tell scientists a lot about the universe.

The occurrence of supernovae reveals to scientists that we live in an expanding universe that is growing at an ever-increasing rate. Scientists have also discovered that supernovae play a vital role in the propagation of elements in the universe. When a star is **, it propagates elements and debris into space.

Many of the elements we find on Earth are produced in constant new**. These elements continue to propagate, forming new stars, planets, and everything else in the universe.

When a star dies, it becomes a supernova. When a super-large star is about to end its life, it will undergo a hydrogen-helium fusion mold wheel and eventually become a supernova after answering the letter.

It can happen, and then a supernova will be produced. This means the end of a planet.

It will carry out hydrogen-helium fusion, and then it will **, and eventually become a supernova, which will also release a certain amount of energy.

The Sun, Proxima Centauri, Vega, Cowherd, and many other famous celestial bodies are stars, and they shine and heat to provide continuous energy for their planets. But whatever it is, its energy is finite, otherwise it would violate the law of conservation of energy, and at the end of a star's life, what will happen? Is it disappearing, or is it happening?

In fact, to understand it, it is necessary to divide stars into two categories: massive stars and low-mass stars.

First of all, let's talk about the end of life of small-mass stars: small-mass stars are basically unable to carry out carbon nuclear fusion reactions, and after completing the nuclear fusion reaction of hydrogen, helium, lithium, beryllium, and boron, they will all turn off and become a white dwarf, and the sun is like this, after continuing to react and burning for billions of years, it will expand first - when the sun becomes a red giant, it will swallow Mercury, Venus, and the Earth, and expand into the orbit of Mars, and at that time, Jupiter will become the closest planet to the sun, and the earth will no longer be suitable for life, and then, it will shrink againto become a white dwarf.

So, after the star stops the fusion reaction, it has no force to resist gravity, so why doesn't it continue to shrink and become an infinitesimal singularity? That's because of the degeneracy of electrons, when the star expands and contracts, the electrons outside the atom will suffer, and they can only stand up to resist this gravitational force.

However, gravity is not vegetarian, and this method is only useful if it is less than or equal to the mass of the Sun, which is called the Chandrasekhar limit, so many white dwarfs will develop type ia supernovae after absorbing material from their companion stars.

When the electron is not empty, it will be pressed into the nucleus by gravity, and the electron will combine with the proton to become a neutron, and the neutron also has degenerate pressure, which can resist gravity and become a neutron star, but this is only limited to a star with 3 times the mass of the sun.

After exceeding 3 times the mass of the sun, the atoms will be crushed and become quarks, which also have degenerate pressure, can resist gravity, and become a quark star. However, there is no observational evidence for quark stars, and the mainstream theory is that after more than 3 times the mass of the sun, it will become a black hole, a real eat-up little expert, which can swallow light.

However, their formation requires a supernova explosion, but white dwarfs do not.

Perhaps, you can also see that from stars, to white dwarfs, neutron stars, quark stars, and black holes, the density of celestial bodies is on the rise, and I can tell you: the density of white dwarfs is 10 million cubic meters, 1 cubic centimeter of neutron star matter weighs between 80 million and 2 billion tons, and the average density of black holes is about 200 million tons per cubic centimeter. It can be seen from this that the celestial bodies are really huge, and human beings are really small.

What's next: What are the types of celestial bodies? There are too many classifications of celestial bodies.