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Radioactive decay (also known as nuclear decay, radioactivity, radioactive disintegration, or nuclear disintegration) is the process by which an unstable atomic nucleus loses energy by radiation. A material containing unstable nuclei is considered radioactive. Three of the most common types of decay are alpha, beta, and gamma decay.
Decay heat is the heat released as a result of radioactive decay. This heat is produced as an effect of radiation on materials: the energy of the alpha, beta or gamma radiation is converted into the thermal movement of atoms. Decay heat occurs naturally from decay of long-lived radioisotopes that are primordially present from the Earth's formation.
About 50% of the Earth's internal heat originates from radioactive decay. [17] Four radioactive isotopes are responsible for the majority of radiogenic heat because of their enrichment relative to other radioactive isotopes: uranium-238 (238 U), uranium-235 (235 U), thorium-232 (232 Th), and potassium-40 (40 K). [18]
The four most common modes of radioactive decay are: alpha decay, beta decay, inverse beta decay (considered as both positron emission and electron capture), and isomeric transition. Of these decay processes, only alpha decay (fission of a helium-4 nucleus) changes the atomic mass number ( A ) of the nucleus, and always decreases it by four.
Radioactive decay is the process in which an unstable atomic nucleus loses energy by emitting ionizing particles and radiation. This decay, or loss of energy, results in an atom of one type (called the parent nuclide ) transforming to an atom of a different type (called the daughter nuclide ).
The decay scheme of a radioactive substance is a graphical presentation of all the transitions occurring in a decay, and of their relationships. Examples are shown below. It is useful to think of the decay scheme as placed in a coordinate system, where the vertical axis is energy, increasing from bottom to top, and the horizontal axis is the proton number, increasing from left to right.
Once 56 Ni is formed it subsequently decays to 56 Co and then 56 Fe by β+ decay. [12] The radioactive decay of 56 Ni and 56 Co supplies much of the energy for the light curves observed for stellar supernovae. [13] The shape of the light curve of these supernovae display characteristic timescales corresponding to the decay of 56 Ni to 56 Co and ...
The shorter-lived 137m Ba (half-life 2.55 minutes) arises as the decay product of the common fission product caesium-137. Barium-114 is predicted to undergo cluster decay, emitting a nucleus of stable 12 C to produce 102 Sn. However this decay is not yet observed; the upper limit on the branching ratio of such decay is 0.0034%.