Nuclear Reactions)
2015
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27 pages
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Abstract
What sort of fusion are we talking about? We started this talking 16 years ago yesterday!
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Fusion power, solution to the global energy crises in 21 st century Introduction to Fusion Even before the development of nuclear energy, scientists realized that a type of nuclear reaction different from the fission was theoretically possible as a source of nuclear energy. Instead of using the energy released as a result of fission of fissile materials like Uranium and Plutonium, the liberation of energy in the fusion reaction of hydrogen isotopes is possible. In fact, this process is the opposite of fission since it involves the fusing together of the nuclei of hydrogen isotopes. It is for this reason that the energy generation based on nuclear fusion is often called nuclear fusion energy. Of the three isotopes of hydrogen the two heaviest species, Deuterium and Tritium, combine most readily to form Helium. Although the energy released in the fusion process per nuclear reaction is less than fission, the same quantity of hydrogen isotopes contains many more atoms than fissile materials. Thus the energy released from hydrogen isotopes fuel is almost four times as much as fissile materials and also 10 million times more than fossil fuels. Of course, this estimation is based on the complete fusion of all hydrogen isotopes atoms. Fusion reactions occur only at extremely high temperatures about 15 million °C, and the rate of reaction increases enormously with the increase in temperature. Such nuclear reactions are known as thermonuclear reaction. Strictly speaking, the term thermonuclear implies that the energy release of nuclei is highly dependent on the temperature, and high temperature plays an important role in proceeding of fusion reaction. Development of fusion reaction is possible only at high temperatures because a huge amount of heat is necessary to trigger fusion through the collision of isotopes of hydrogen nuclei. To start the fusion reaction, the repulsion of positively charged nuclei has to be ovileercome. When the nuclei get close enough to touch, the strong nuclear force becomes the dominant force. This is exactly the process that happens in the inner core of the sun, where the temperature is about 15
2021
We will burn coal, oil and gas in the next 100 years. There is not much uranium on Earth. We can only hope for a fusion reaction. The problem is the absence of a physical model of the micro world. There is still time to do it. 70 years wasted In 1935, Hans Bethe suggested that the source of solar energy could be the thermonuclear reaction of converting hydrogen to helium, for which he won the Nobel Prize in 1967. In 1950 I.E. Tamm and A.D. Sakharov proposed to carry out controlled thermonuclear fusion in a toroidal chamber with a
Physics Letters B, 1989
Charge distributions, kinetic energy spectra, and angular distributions were measured for the reverse kinematics reactions, 19.7 MeV/nucleon S°Ar+ ~2C, 27A1. Invariant cross section plots constructed in the VrV± plane give a global view of the several competing reaction mechanisms. The evaporation residue cross section, which dominates the fusion cross section for the 4°At+ ~2C reaction, decreases dramatically in the 4°Ar+27A1 reaction and is replaced by isotropic binary decay, arising presumably from compound nucleus decay.
Even before the development of nuclear energy, scientists realized that a type of nuclear reaction different from the fission was theoretically possible as a source of nuclear energy. Instead of using the energy released as a result of fission of fissile materials like Uranium and Plutonium, the liberation of energy in the fusion reaction of hydrogen isotopes is possible. In fact, this process is the opposite of fission since it involves the fusing together of the nuclei of hydrogen isotopes. It is for this reason that the energy generation based on nuclear fusion is often called nuclear fusion energy. Of the three isotopes of hydrogen the two heaviest species, Deuterium and Tritium, combine most readily to form Helium. Although the energy released in the fusion process per nuclear reaction is less than fission, the same quantity of hydrogen isotopes contains many more atoms than fissile materials. Thus the energy released from hydrogen isotopes fuel is almost four times as much as fissile materials and also 10 million times more than fossil fuels. Of course, this estimation is based on the complete fusion of all hydrogen isotopes atoms. Fusion reactions occur only at extremely high temperatures about 15 million °C, and the rate of reaction increases enormously with the increase in temperature. Such nuclear reactions are known as thermonuclear reaction. Strictly speaking, the term thermonuclear implies that the energy release of nuclei is highly dependent on the temperature, and high temperature plays an important role in proceeding of fusion reaction. Development of fusion reaction is possible only at high temperatures because a huge amount of heat is necessary to trigger fusion through the collision of isotopes of hydrogen nuclei. To start the fusion reaction, the repulsion of positively charged nuclei has to be ovileercome. When the nuclei get close enough to touch, the strong nuclear force becomes the dominant force. This is exactly the process that happens in the inner core of the sun, where the temperature is about 15
Harnessing fusion-energy is something theoretically impossible, and not a technological problem. Energy production requires spontaneous changes, whereas nuclear fusion is nonspontaneous on Earth. In this paper, I explain in a simple way why it is non-spontaneous, by comparing it with the spontaneous changes involved in the existing power plants (hydroelectric, fission and thermal). The difference between fission and fusion is that in the former, energy 'flows out', but in the latter, energy is 'squeezed out'.
This research presents a proof of Legendre's conjecture using the concept of maximum prime gaps. The conjecture posits that for every positive integer 𝑛, there exists at least one prime number in the interval between 𝑛 2 and (𝑛 + 1) 2. This work not only reinforces the conjecture but also explores the relationship between prime gaps and prime densities, thereby contributing to the broader understanding of prime number distribution.
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