Nuclear Fusion

Fusion reactions can occur in laboratories through devices like tokamaks and inertial confinement fusion reactors. These devices use controlled conditions to generate the extreme temperatures and pressures needed for fusion to take place.

If you mean used by humans, this would have been the first H-bomb test, I'm not sure of the date.

Greenhouse George test in 1950, yield 225KTon, verified feasibility by "lighting a fusion match using a fission blast furnace". Probably much less than 1KTon of yield was due to fusion.

Ivy Mike test in 1952, yield 10MTon, erased the island of eugelab in eniwetok atoll. Device was 80 foot tall, 20 foot diameter, 2 foot thick steel case containing triple steel thermos filled with cryogenic liquid deuterium/tritium and an atomic bomb at the bottom below the thermos.

In 1953 the soviets did an H-bomb test, using solid lithium-deutride fuel in the first actual thermonuclear airdrop, but it was a different design that could not yield much more than a few megatons max.

The US Castle Bravo test in 1954, yield 15MTon, on the end of a causeway at eniwetok atoll punched a hole in the outer reef. Device was first solid lithium-deutride fueled bomb using principles of Ivy Mike design. 5MTon of yield was due to a totally unanticipated effect of the Lithium-7 isotope in the lithium-deutride.

Most of the rest of the high yield Castle and 1956 Redwing tests were either done as airdrops or barge tests in lagoon or Ivy Mike crater to limit further damage to the finite atoll landmass. (how considerate)

It's the process that takes place in the cores of stars, creating heavier elements

out of lighter ones, and liberating nuclear energy that leaves the stars in the form

of electromagnetic radiation.

The nuclear fusion in the sun smashes hydrogen atoms together. The atoms do not combine easily and the fusion (combining of two atoms) can only happen under tremendous pressures by the weight of the material (the gravitational pressures of the star due to its large mass).

Here are the steps.

1. Two pairs of hydrogen protons to form 2 deuterons (a hydrogen isotope)

2. Each deuteron fuses with an additional proton of hydrogen to form helium-3

3. Two helium-3 nuclei fuse to create beryllium-6, but this is unstable and disintegrates immediately into two protons and a helium-4

4. the two protons, together with other hydrogen protons, can then form 2 deuterons and the process starts again.

Whenever the fusion takes place, mass is "destroyed" as the result is energy which is released through radiation.

The above method is the primary nuclear reaction in our sun. There is also an alternate method which larger stars use called the CNO cycle, but it requires a much larger mass than our sun (about 50% larger) to initiate.

To make fusion a source of energy we would need to be able to get hydrogen to start moving extreamly fast and that would take heating it up to 1,000,000 degrees and we cannot do that How to sustain the reaction for an indefinite period of time. We are currently able to hold a fusion reaction for just a few nanoseconds,

Actually room temperature nuclear fusion has been verified by reputable scientists, but it only works with muonic-hydrogen. This is hydrogen with its electron replaced by a muon, a particle identical to the electron except that it weighs 200 times as much. Because of the extra mass the muon orbits the proton much closer than the electron does. This allows muonic-hydrogen nuclei to collide and fuse at room temperature.

However it takes far more energy to make the muons and replace them for the electrons than can be obtained from the fusion.

The main challenges of using nuclear fusion for electricity generation include controlling the high temperatures and pressures required for fusion reactions, sustaining the reaction over long periods, and developing materials that can withstand the intense radiation produced. Research is ongoing to overcome these challenges and develop practical fusion reactors for commercial electricity production.

In nuclear fusion, the mass of the atomic nuclei is converted into energy according to Einstein's famous equation E=mc^2. This means that a small amount of mass is converted directly into a large amount of energy during the fusion process.

Nuclear fusion is the process by which lighter atoms combine to form heavier ones, releasing a large amount of energy. This process occurs in the cores of stars, where elements are formed through the fusion of hydrogen into helium and subsequently into heavier elements. The fusion reactions in stars are responsible for creating most of the elements found in the universe through nucleosynthesis.

Nuclear fusion in stars involves the fusion of lighter elements to form heavier elements, releasing energy in the process. As stars evolve, they undergo processes like supernova explosions, which can produce even heavier elements through nucleosynthesis. This gradual accumulation of heavier elements in stellar environments eventually leads to the formation of all the chemical elements.

Uranium is fairly easy to obtain, and the 235 isotope can be separated or increased, which is the fissile one. The only alternative is plutonium, and that has to be separated out from used uranium fuel. In some countries, but not the US, this has been done and a mixed uranium/plutonium fuel produced.

A nuclear fusion reactor works by creating high temperatures and pressures to fuse atomic nuclei together, releasing vast amounts of energy in the process. The reaction itself happens very quickly, with fusion reactions occurring on the order of microseconds. However, sustaining and controlling the reaction to generate continuous energy requires sophisticated equipment and technology.

In a star, nuclear fusion occurs in multiple stages. The main sequence stars, like our sun, primarily fuse hydrogen into helium in their cores through the proton-proton chain reaction. As the star evolves, it can go on to fuse heavier elements like carbon, oxygen, and eventually iron through various nuclear reactions.

The nuclear fusion order for a star like our Sun involves the conversion of hydrogen into helium. This fusion process occurs in multiple stages, beginning with the fusion of hydrogen isotopes (protons) into deuterium, and then further reactions combine deuterium to form helium-3 and, ultimately, helium-4.

Building a fusion reactor is a complex engineering challenge that requires controlling extremely high temperatures and pressures. Research is ongoing, but the technology is not yet mature enough for practical implementation on a large scale. Additionally, funding and resources for fusion research have been limited compared to other energy sources.

Two protons would be particle unstable, so one of them must change to a neutron.

This will always produce a deuteron, a positron and an (electron)neutrino and a gamma ray will be emitted.

This is true for the simple p-p chain which is predominant in the Sun, and also in the CNO cycle which is a minor component of the Sun's fusion but important for more massive stars.

Existing element is product of nuclear fusion, heavy element exist from over fusion and thus create high atomic mass substance. To answer what is the element that is form last in nuclear fusion in star is the same as asking what is the heaviest element occur or found in nature.

Base on what is in periodic table. The heaviest element found naturally is around Uranium - Plutonium thus it could be considered the last product known in nuclear fusion in star.

There are heavier element than Uranium and Plutonium but those are synthesize element. Nuclear fusion might go to element heavier than what is known in our periodic table but those substance may be unstable and decay over time until none of those exist.

Nuclear fusion is the coming together of two nuclei to form a different element whereas the combining of two hydrogen atoms to form H2 gas is just a chemical reaction where a covalent bonds form between two hydrogen atoms. Nuclear fusion involves combining of two nuclei whereas in the covalent bond formation the electrons of the hydrogen atoms interact with each other.

Nuclear fusion is not yet a controlled reaction on Earth because it requires extremely high temperatures and pressures to overcome the electrostatic repulsion between positively charged atomic nuclei. Current technology is still unable to sustain these conditions reliably and efficiently for energy production. Scientists are working on developing fusion reactors, but more research and technological advancements are needed to achieve practical fusion energy.

No, a nuclear power plant producing electricity is an example of nuclear fission, not fusion. In nuclear fission, the nucleus of an atom is split, releasing energy, whereas in nuclear fusion, atomic nuclei combine to release energy.

Nuclear fusion is the process by which stars generate energy by fusing lighter elements into heavier ones. In the life cycle of a star, nuclear fusion occurs in the core and provides the energy necessary to counteract gravitational forces and maintain the star's equilibrium. As a star exhausts its nuclear fuel, it may undergo different stages of fusion, eventually leading to its death.

In nuclear fusion, a small amount of heat is generated due to the high temperatures required to fuse atomic nuclei together. This heat can be harnessed to produce electricity through various methods, such as heating water to create steam to drive a turbine. However, the amount of energy produced by fusion reactions is significantly greater than the heat generated.

A helium nucleus plus energy released. see the link below

A massive star with iron in its core will stop nuclear fusion, leading to its collapse and eventual explosion as a supernova. Iron is the element at which fusion becomes endothermic, meaning energy is no longer released in the process.

In the core of the Sun, hydrogen atoms fuse to form helium in a process known as hydrogen fusion. This is the primary fusion process occurring in the Sun. As the core hydrogen is depleted, helium fusion into heavier elements like carbon and oxygen will occur in later stages of the Sun's evolution.