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Fusion Of The Sun And Stars And Nuclear Fusion

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Nuclear Physics

The Process of Solar Fusion

Their was and still continues to be plenty of quarrels among the scientific community over the two types of sciences known as geology and astronomy. The science of astronomy is the study of the make up of the solar system as well as the entire universe. The science of geology is the study of the history of the earth, which may be seen in some of the features of the earth as depicted in rocks or in fossils. It is also the study of the geological features of the earth. Many people may not agree with the fact that the universe is billions of years old, although there is plenty of evidence to support this. The reason why people may not support the theory that universe is so ancient is because the fact that the theory of the universe being so old contradicts the religious beliefs of many people. The massive amount of evidence such as how the sun heats up and how long it lasts clearly leads many scientists to believing that the age of the sun, much less the universe is millions and millions of years old. Their was and will continue to be a lot of controversy on the interesting subjects of both astronomy and geology.  

 

Here is the diagramatic representation of our insignificance in our Milky Way Galaxy, much less the entire universe:

  

  The above picture had been downloaded from google.

Albert Einstein discovered an equasion which equates the energy to the mass of and object, multiplyed by the speed of lif squared That, in addition to the unearthing of radioactivity at approximately the same time, made many scientists to have new ideas regarding the sun's heat. A pretty famous astronomer Henry Norris Russell speculated. about the properties that the sun's mysterious heat source must have originated from and made several surprisingly, accurate conclusions. But it appears to have been Sir Arthur Eddington, Einstein's american fellow physicist, who first noticed the mass deficit of helium as compared to hydrogen, and suggested the fusion of hydrogen into helium might be the ultimate source of the sun's power

 

One day, however, Albert Einstein derived the surprising equivalence between mass and energy (E=mc2) as a curious side effect of special relativity theory. That, plus the discovery of radioactivity at about the same time, led to new ideas about the sun's heat. A pretty famous astronomer Henry Norris Russell speculated about the properties that the sun's mysterious heat source must have originated from and made several surprisingly, accurate conclusions. But it appears to have been Sir Arthur Eddington, Einstein's american fellow physicist, who first noticed the mass deficit of helium as compared to hydrogen, and suggested the fusion of hydrogen into helium might be the ultimate source of the sun's power.

 

 

 

The above picture has been downloaded from google.

 

It is Hans Bethe who usually gets credit for first proving the amazing process of nuclear fusion as the sun's energy source, beyond Eddington's level of speculation, in a one page letter to the editor of Physical Review. This paper became the beginnings of Chandrasekhar's book, which really established the full scale of mathematical physics in stellar structure and evolution. But Bethe's work came too late, after the relevant chapters of Chandrsekhar's book were already written. 

 

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the above has been downloaded from google:

But while the basic theories of how molecules and atoms seemed to work, somethings amazing known as reaction rates and reaction channels remained unknown. The post WWII boom in nuclear physics, sparked by war research and the Manhatten Project, changed all of that. With the new knowledge firmly in hand, it could finally be determined, once and for all, if nuclear fusion would really generate the needed energy fast enough to serve as the energy source for stars. The answer was yes. Here is a really cool representation of nuclear fusion in the sun:

 

 The above picture has been downloaded from google:

All of this work established the theories of the amazing reality of fusion powered stars, but only stellar surface could be observed, not stellar interiors. That has since changed, with the creation of sciences known as helioseismology and neutrino astronomy, both of which allow us to peer into the solar interior.

Pre Main Sequence Collapse

The standard model of stellar birth has long maintained that stars are the end result of the gravitational collapse of large clouds of dust and gas. These clouds are well known to exist, and are indeed prevalent throughout this galaxy, and all other galaxies we can see in sufficient detail.

 

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 The above had been downloaded from google.

The exact mechanism of collapse and star formation remains the topic of considerable discussion amongst astrophysicists. However, that the overall model is correct was confirmed by a series of dramatic images returned by the Hubble Space Telescope. Her is an example and representation of this: 

video previewthis had also been downloaded from google.

The collapse of a great cloud into a star or a cluster of stars is not a mystery. The force that does it is gravity. The outer parts of the clouds fall inward as a result of their own weight. That weight is very small, but not zero. It happens, but it takes time.

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 This has also been downloaded from google.

As the protostar collapses, the interior of the collapsing cloud naturally heats up. As the temperature rises, the speed with which the particles that make up the cloud collide with each other also rises. As the collisions become more energetic, the atoms deep inside the cloud collide so strongly that the electrons are stripped away from all of the nuclei. The gas becomes a completely ionized plasma, a mix of free electrons and free atomic nuclei, the vast majority of which are hydrogen nuclei, which are protons. Eventually, the temperature gets high enough for the protons to stick together. That's when proton fusion begins, and that's when the collapsing cloud becomes a true star.

 

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The above had been downloaded from google.

This website is for my Secondary Semester Research Project for Geoscience Perid 2. Teacher: Mrs. Van Pelt

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Energy Production in the Sun by Nuclear Fusion
Matter is made of atoms

Here is a tour of the atomic world.

We need to know the players in the game and the rules -- that is the particles and their interactions.

The middle of the Sun is a very hot gas. It is ionized: all of the electrons have been ripped away from the nuclei because it is so hot. The nuclei available are mostly 1H, quite a lot of 4He, and a few 2H and 3He. (There are a few other types, but they are not so important for us.)

What is happening in the middle of the Sun is analogous to burning methane:


C H4 + 2 O2 --> C O2 + 2 H2 O
In this reaction, the final molecules have less internal energy than the starting molecules. Since energy is conserved, the extra energy is released as energy of motion of the molecules. That is the gas gets hotter. The amount of energy involved is 5.5 eV each time the reaction above happens.
As we have seen, much more energy than that must be involved in the reactions inside the Sun and other stars. The evidence is strong that the overall reaction is "burning" hydrogen to make helium:

4 1H + 2 e --> 4He + 2 neutrinos + 6 photons
In this reaction, the final particles have less internal energy than the starting particles. Since energy is conserved, the extra energy is released as energy of motion of the nuclei and electrons in the solar gas, the production of lots of low energy photons and, finally, the energy of the neutrinos, which just zip right out of the Sun. That is the gas gets hotter and has lots of photons (and neutrinos). The amount of energy involved is 26 MeV = 26 x 106 eV each time the reaction above happens.
Why do we think that this is what goes on?

Energy output of millions of eV per reaction is needed if the Sun has been producing energy at the observed rate over billions of years.
The reactions exist. (They have been studied in the laboratory.)
There is a consistent step-by-step theory for the reaction. (We will study this a bit.)
The reaction as given above is a summary. The step-by-step picture is illuminating.

Davison E. Soper, Institute of Theoretical Science, University of Oregon, Eugene OR 97403 USA soper@bovine.uoregon.edu