Why does helium accumulate in the sun s core instead of spreading?

This is due to its physical properties. The sun's transformation into a red giant is the hypothetical plot premise of today's science fiction movie "The Wandering Earth", because when the sun has a helium flash, it means that it is about to move towards the process of becoming a red giant, and the volume of the sun at this time will enter a stage of rapid expansion, and eventually its volume will be equivalent to millions of times the volume of the sun today.

In our solar system, the sun itself is a behemoth, its diameter has reached 1.39 million kilometers, 1.3 million times larger than our earth, the combined volume of the eight major planetary bodies is less than 1,500, and its mass accounts for the amount of visible matter in the entire solar system.

Why does the Sun expand in size like this? It is because the structure of the sun and the fusion combustion of hydrogen and helium are different, the fusion of hydrogen in the sun mainly occurs in the inner 1 4 region, and the outer range mainly belongs to the radiation zone, now the sun is fusing and burning hydrogen, and the hydrogen element becomes helium after combustion, but due to the blocking of the peripheral radiation zone, helium will not diffuse to the entire sun, so helium will accumulate in the core of the sun, and in this process, the sun is also in a state of continuous heating.

One day, the pressure and temperature inside the sun and the accumulation of helium can reach the level of helium flash, at this moment helium will be ignited and fused, and the energy release is very violent, which can be said to be second only to supernova explosions, and the intensity can vaporize some nearby planet surfaces, at this time, if the earth is still in the existing orbit, the ecological environment on the surface will be destroyed instantly. So in the movie "The Wandering Earth", humans launched the "Wandering Earth" program hundreds of years before the helium flash broke out of the sun, driving the earth out of the solar system and going to the vicinity of Proxima Centauri to find a new home.

After the helium flash, the helium element in the core of the sun enters the continuous fusion combustion phase, but in the periphery of the helium fusion combustion area, the hydrogen element is still fusing and burning, and the fusion combustion of these two elements will greatly increase the outward radiation pressure of the sun, so the volume of the sun will be in the expansion stage, and the outer gas shell will also spread far away, so the size of the sun will increase dramatically. Astronomers believe that the diameter of the Sun will increase by about 110,150 times, and its volume will increase to between 130,380,000 times that of today.

The diameter of the sun is 1.39 million kilometers, and the diameter of the expanded sun will reach 100 million kilometers, and our earth is about 100 million kilometers away from the sun.

Often, deuterium collides with wandering protons to produce helium-3. Helium-3 is a stable isotope of helium, and it can also accumulate in the sun's core. Because helium-3 has two protons, it is difficult for protons to collide with helium-3.

In the case of zero gravity in space, if there is no thrust, he will not spread very far.

Helium and hydrogen collide in the core of the sun.

Because he's going to collide with the hydrogen in the sun.

Helium-3 is a stable isotope of helium.

Only when they are gathered together can they be used better.

Because it is easier to store the glow when gathered.

Because the sun has a gravitational pull and helium is heavier than hydrogen, helium is concentrated in the center.

Maybe it's because it's spread out and it's not easy to use.

This is because it reacts inside the sun.

Astronomers have observed a gas in the universe leaking its own helium into space as it orbits a bright star. For more than a decade, astronomers have been looking for elements released by gas giants. Laura Kridberg, an exoplanetary astronomer at Harvard University in the United States, said that the first discovery of helium on an exoplanet is very exciting.

The discovery of helium was a fortuitous process, as scientists were looking for methane in the atmosphere of the gas giant, which was later discovered to contain helium.

This gas giant is about the size of Jupiter, but only one-eighth the mass of Jupiter, making it one of the least dense exoplanets known. Jessyca, an astronomer at the University of Exeter in the United Kingdom who studies extrasolar planets, thinks there could be more, and it will be a daunting task. Helium is the second most abundant element in the universe, the first being hydrogen.

Initially, they were confused about the meaning of the chemical element, but eventually they determined that it was helium. Since the spike is caused by the "transferable" form of helium, the energy can be sustained. Fortunately, the observed gas giant WASP-107B is able to combine a fluffy atmosphere with an orbit and then use the star's radiation to make helium metastable and therefore easier to capture.

For the first time outside the solar system, the detected gas giant WASP-107B was able to combine a fluffy atmosphere and orbit, and then turn helium into a metastable state through the radiation of the star.

The helium detected for the first time exists in the form of a gas in space, and it does not liquefy and is stable in form.

The first detection of the presence of helium was detected by scientists, many of whom were discovered when they were unknown.

In the early stage of solar nuclear fusion, protons and protons collide with each other, and the fusion of two protons releases a positron and a neutrino to generate a deuterium nucleus (including a neutron and a proton). If this deuterium nucleus collides with a third proton, it is possible to produce a nucleus of another element, a helium nucleus containing one neutron and two protons, which is 3he. Although the probability of a continuous collision of these three hydrogen nuclei is very small, the mass of the sun is very large, and the number of protons is naturally innumerable, so the mass of the produced HE is still very impressive.

If two of the above 3He nuclei collide, a true 4He nucleus may be produced with 2 neutrons and 2 protons. 2 protons are released at the same time. These two protons have the opportunity to participate in a new round of nuclear fusion of proton chains.

Nuclear fusion refers to the small mass of atoms, mainly deuterium or tritium, under certain conditions (such as ultra-high temperature and high pressure), only at extremely high temperature and pressure can the electrons outside the nucleus get rid of the bondage of the nucleus, so that the two nuclei can attract each other and collide together, the nuclei polymerize with each other, and generate a new heavier nucleus (such as helium), although the neutron mass is relatively large, but because the neutron is not charged, it can also escape from the bondage of the nucleus and release it in the collision process, The release of a large number of electrons and neutrons is manifested by a huge release of energy.

Deuterium and tritium are both isotopes of deuterium (i.e., ordinary hydrogen atoms), both have only one proton, but contain neutrons (ordinary hydrogen atoms have no neutrons), and deuterium and tritium attract each other to form a new element with two protons (i.e., helium).

The reason for the huge amount of energy released is the loss of quality.

The sun will run out of hydrogen in the core. Massive stars will deplete their cores of hydrogen faster than their smaller ones. After the hydrogen in the core is consumed, the nuclear reaction in the core stops, leaving behind a helium nucleus.

After losing the energy of the nuclear reaction against gravity, the outer shell of the star begins to collapse gravitationally. The temperature and pressure of the core are elevated as during star formation, but at a higher level. Once the temperature of the core reaches 100 million degrees Kelvin, the core begins helium fusion, which regenerates energy to resist gravity.

Stars that are not massive enough to produce helium fusion release heat energy that gradually cools down and becomes white dwarfs.

Because it requires greater temperatures, the difficulty of nuclear fusion increases exponentially as the elements get bigger. Therefore, metal elements are formed under extremely unimaginable conditions, so the content is much less.

This is directly related to the structure of the sun, after the helium flash will not only become larger, but also the temperature will increase, resulting in more frequent internal activities of the sun, and the solar wind and sunspots will also frequently erupt, affecting the surrounding stellar environment.

It doesn't matter, any star will experience a helium flash.

First of all, the essence of helium flash is: the essence of solar combustion is the fusion of hydrogen nuclei, and the nuclear fusion releases energy at the same time to form helium atoms. As the sun continues to undergo nuclear fusion, resulting in increasing temperature and pressure until the conditions for the fusion of helium nuclei are reached, the helium atoms are ignited, releasing a large amount of energy, and a helium flash is formed.

The increase in volume is due to the fact that the fusion of helium nuclei and the remaining fusion energy of hydrogen nuclei are superimposed, and the radiation pressure released outward is greatly enhanced, causing the sun to expand extremely quickly. The size of the expansion is related to the number of accumulated helium atoms, and scientists have speculated that the volume of the sun will become 1.4 million to 3.8 million times the original after the helium flash.

Relate. The reason why the sun becomes larger after the helium flash is due to the difference in the structure of the sun and the fusion combustion of hydrogen and helium.

1) According to the conservation of charge number and mass, the nuclear reaction equation is: 4h

he+2e2) has a mass deficit of m=4mh

mhe2me

Then the energy released e= mc2(4mh

mhe2me

C Answer: (1) The nuclear reaction equation is: 4

hhe+2e2) The energy released by a nuclear reaction is (4mhm

he2mec