![]() ![]() It has been shown by a scientist Eddington in 1920 that four hydrogen can be fused together to form a helium atom. The nuclear reaction that is mentioned above is termed as nuclear fusion. A positive Q value is the result obtained from it that signifies a release of energy. This is the reason if two lighter nuclei get fused together to form a heavy nucleus then the binding energy would have a greater value and the nuclear mass would decrease consequently. Nuclear binding energy curve from wikipedia Let’s come to the core of this concept i.e, the bindinding energy per nucleon.Īccording to the binding energy curve, comparatively lighter nuclei that are placed on the steep portion of the curve have lesser values of binding energy per nucleon than the binding energy per nucleon of the nuclei of intermediate mass numbers. In case of fusion two lighter nuclei combine to form a heavier nucleus. We all know that when a heavy nucleus of uranium 235 breaks into two fragments of two different lighter nuclei of barium and krypton accompanied by 3 faster neutrons then this reaction is known as nuclear fission. Nuclear fusion is just the opposite reaction of nuclear fission. A large, exploding star or supernova releases the energy needed to fuse all of the heavier elements.In this article the nuclear fusion process is going to be illustrated step by step with explanations and facts related to it.īefore starting the detailed facts related to nuclear fusion process we should have a basic idea regarding nuclear fusion reaction and how it is different from the nuclear fission reaction. It was from the energy of other explosions. For element heavier than iron, fusion requires energy. The total mass of the helium nucleus is less than the sum of the mass of the 4 particles that make it up.Īdding additional protons and neutrons to iron doesn't release energy because the binding energy peaks at this element. A MeV is equal to 1.602 x 10 -13 joules.Īnother way to think of the energy released by fusion is to look at the change in mass. This is the same amount of energy that is required to break them apart.Įnergy in this table is reported in units of MeV or mega-electron volts. The nuclear binding energy for H-1, a proton, is zero because there is only one particle in the nucleus.Īs the number of particles in the nucleus increases, energy is released. The protons and neutrons are held together through a type of energy called nuclear binding energy. In going from hydrogen to iron, energy is released as nuclei fuse to make bigger ones. This promotes the fusion of heavier and heavier elements, ultimately forming all the elements up to iron. As the hydrogen is used up, the core of the star condenses and heats up even more. The fusion of hydrogen nuclei uses up hydrogen to produce helium and energy. Two He-3 nuclei can fuse to make a nucleus of an unstable beryllium nucleus (Be-6) that breaks apart to give He-4 and two protons. The deuterium nuclei can merge to form a helium nuclei (He-4), or they can interact with other protons to make another isotope of helium (He-3). Under these conditions protons (H-1) react with other protons to make deuterium nuclei (H-2) and positrons. That is, the electrons separate from the nuclei to give a mix of positively charged ions and electrons. At this temperature, the hydrogen and helium gases become a plasma. The density of gas in the core of our sun is 160 g/cm 3, much higher than the densest metal, and the temperature is 15,000,000 K (27 million degrees Fahrenheit). In the core of a star, gravity produces high density and high temperature. Isotopes of an element all have the same number of protons but different numbers of neutrons. Each element has a particular number of protons in the nucleus. This produced energy, the heat and light of the stars.įusion a type of nuclear reaction where two nuclei come together to form the nucleus of a different element. The gravitational force at the core brought the matter closer and closer together until some of the nuclei coalesced. Swirls of hydrogen and helium gas condensed into huge clouds. ![]()
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