A supernova is the explosion of a star -- the largest explosion that takes place in space. Its most stable isotope U-238 is radioactive with a half-life of 4.5 billion years, similar to the age of the Earth. This explosion was produced by a type Ia supernova, which is theorized to be triggered in binary systems consisting of a white dwarf and another star—and could be a second white dwarf, a star like our Sun, or a giant star. Supernovae are one of the most energetic explosions in nature, equivalent to the power in a 10 28 megaton bomb (i.e., a few octillion nuclear warheads).. Types of Supernovae Elements lighter than iron can release energy by fusion; elements heavier than iron can release energy by fission; but nothing that you do to iron can release energy. All the stars in the universe, including the Sun, are … Where oxygen and hydrogen meet, you get water. Supernovae, as celestial events, are huge releases of tremendous energy, as the star ceases to exist, with about 10 20 times as much energy produced in the supernova explosion as our Sun releases every second. The dominant, stable form of iron is iron-56, whose nucleus contains 26 protons and 30 neutrons. All the heavier elements up through uranium appear when a star of sufficient mass collapses in a supernova event. The supernova explosion produces a flood of energetic neutrons that barrel through the expanding material. Fusion, which occurs when atomic nuclei combine to form new elements, is extremely powerful. When a star is born , it is because it has enough mass to create enough heat, gravity and pressure to sustain nuclear fusion. The most common elements, like carbon and nitrogen, are created in the cores of most stars, fused from lighter elements like hydrogen and helium. Thus, they can build up elements that are more massive than iron, possibly including such terrestrial favorites as gold, silver and uranium. The supernova event is indicated by the box and the inset. Iron-60 has four extra neutrons. They represent the very final stages of evolution for some stars. Supernovae, as celestial events, are huge releases of tremendous energy, as the star ceases to exist, with about 10 20 times as much energy produced in the supernova explosion as our Sun releases every second. It is radioactive and decays with a half-life of 2.6 million years. Thus, they build up elements that are more massive than iron, including such terrestrial favorites as … Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe.The table shows the lifetimes of stars as a function of their masses. These neutrons can be absorbed by iron and other nuclei where they can turn into protons. If neutrons are added to a stable nucleus, it is not long before the product nucleus becomes unstable and the neutron is converted into a proton. In nuclear astrophysics, the rapid neutron-capture process, also known as the r-process, is a set of nuclear reactions that is responsible for the creation of approximately half of the atomic nuclei heavier than iron; the "heavy elements", with the other half produced by the p-process and s-process.The r-process usually synthesizes the most neutron-rich stable isotopes of each heavy element.
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