Decay energy

This article includes a list of general references, but it lacks sufficient corresponding inline citations. Please help to improve this article by introducing more precise citations. (September 2018) (Learn how and when to remove this message)

Nuclear physics
Nucleus Nucleons p n Nuclear matter Nuclear force Nuclear structure Nuclear reaction
Models of the nucleus Liquid drop Nuclear shell model Interacting boson model Ab initio
Nuclides' classification Isotopes – equal Z Isobars – equal A Isotones – equal N Isodiaphers – equal N − Z Isomers – equal all the above Mirror nuclei – Z ↔ N Stable Magic Even/odd Halo Borromean
Nuclear stability Binding energy p–n ratio Drip line Island of stability Valley of stability Stable nuclide
Radioactive decay Alpha α Beta β 2β 0v β+ K/L capture Isomeric Gamma γ Internal conversion Spontaneous fission Cluster decay Neutron emission Proton emission Decay energy Decay chain Decay product Radiogenic nuclide
Nuclear fission Spontaneous Products pair breaking Photofission
Capturing processes electron 2× neutron s r proton p rp
High-energy processes Spallation by cosmic ray Photodisintegration
Nucleosynthesis and nuclear astrophysics Nuclear fusion Processes: Stellar Big Bang Supernova Nuclides: Primordial Cosmogenic Artificial
High-energy nuclear physics Quark–gluon plasma RHIC LHC
Scientists Alvarez Becquerel Bethe A. Bohr N. Bohr Chadwick Cockcroft Ir. Curie Fr. Curie Pi. Curie Skłodowska-Curie Davisson Fermi Hahn Jensen Lawrence Mayer Meitner Oliphant Oppenheimer Proca Purcell Rabi Rutherford Soddy Strassmann Świątecki Szilárd Teller Thomson Walton Wigner
Physics portal  Category
v t e

The decay energy is the energy change of a nucleus having undergone a radioactive decay. 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 energy difference of the reactants is often written as Q:

${\displaystyle Q=\left({\text{Kinetic energy}}\right)_{\text{after}}-\left({\text{Kinetic energy}}\right)_{\text{before}},}$

${\displaystyle Q=\left({\text{Rest mass}}\right)_{\text{before}}c^{2}-\left({\text{Rest mass}}\right)_{\text{after}}c^{2}.}$^[1]

Decay energy is usually quoted in terms of the energy units MeV (million electronvolts) or keV (thousand electronvolts):

${\displaystyle Q{\text{ [MeV]}}=-931.5\Delta M{\text{ [Da]}},~~({\text{where }}\Delta M=\Sigma M_{\text{products}}-\Sigma M_{\text{reactants}}).}$^[2]

Types of radioactive decay include

• gamma ray
• beta decay (decay energy is divided between the emitted electron and the neutrino which is emitted at the same time)
• alpha decay

The decay energy is the mass difference Δm between the parent and the daughter atom and particles. It is equal to the energy of radiation E. If A is the radioactive activity, i.e. the number of transforming atoms per time, M the molar mass, then the radiation power P is:

${\displaystyle P=\Delta {m}\left({\frac {A}{M}}\right).}$

or

${\displaystyle P=E\left({\frac {A}{M}}\right).}$

or

${\displaystyle P=QA.}$

Example: ⁶⁰Co decays into ⁶⁰Ni. The mass difference Δm is 0.003 u. The radiated energy is approximately 2.8 MeV. The molar weight is 59.93. The half life T of 5.27 year corresponds to the activity A = N [ ln(2) / T ], where N is the number of atoms per mol, and T is the half-life. Taking care of the units the radiation power for ⁶⁰Co is 17.9 W/g

Radiation power in W/g for several isotopes:

⁶⁰Co: 17.9

²³⁸Pu: 0.57

¹³⁷Cs: 0.6

²⁴¹Am: 0.1

²¹⁰Po: 140 (T = 136 d)

⁹⁰Sr: 0.9

²²⁶Ra: 0.02

For use in radioisotope thermoelectric generators (RTGs) high decay energy combined with a long half life is desirable. To reduce the cost and weight of radiation shielding, sources that do not emit strong gamma radiation are preferred. This table gives an indication why - despite its enormous cost - ²³⁸
Pu with its roughly eighty year half life and low gamma emissions has become the RTG nuclide of choice. ⁹⁰
Sr performs worse than ²³⁸
Pu on almost all measures, being shorter lived, a beta emitter rather than an easily shielded alpha emitter and releasing significant gamma radiation when its daughter nuclide ⁹⁰
Y decays, but as it is a high yield product of nuclear fission and easy to chemically extract from other fission products, Strontium titanate based RTGs were in widespread use for remote locations during much of the 20th century. Cobalt-60 while widely used for purposes such as food irradiation is not a practicable RTG isotope as most of its decay energy is released by gamma rays, requiring substantial shielding. Furthermore, its five-year half life is too short for many applications.

• Q value (nuclear science)

• Radioactivity Radionuclides Radiation by Joseph Magill and Jean Galy, Springer Verlag, 2005