Uranium-235

Template:Short description Template:Redirect Template:Infobox isotope Uranium-235 (Template:SimpleNuclide or U-235) is an isotope of uranium making up about 0.72% of natural uranium. Unlike the predominant isotope uranium-238, it is fissile, i.e., it can sustain a nuclear chain reaction. It is the only fissile isotope that exists in nature as a primordial nuclide.

Uranium-235 has a half-life of 704 million years. It was discovered in 1935 by Arthur Jeffrey Dempster. Its fission cross section for slow thermal neutrons is about Template:Val barns.<ref name="StandardReactionIAEA">Template:Cite web</ref> For fast neutrons it is on the order of 1 barn.<ref>Template:Cite web</ref> Most neutron absorptions induce fission, though a minority (about 15%) result in the formation of uranium-236.<ref name=power-ratio>Template:Cite web</ref><ref name=ratio-1962>Template:Cite journal</ref>

Fission properties

Nuclear fission seen with a uranium-235 nucleus

The fission of one atom of uranium-235 releases Template:Val (Template:Val) inside the reactor. That corresponds to 19.54 TJ/mol, or 83.14 TJ/kg.<ref name="kayelaby">Nuclear fission and fusion, and neutron interactions, National Physical Laboratory Archive.</ref> Another 8.8 MeV escapes the reactor as anti-neutrinos. When Template:Chem nuclei are bombarded with neutrons, one of the many fission reactions that it can undergo is the following (shown in the adjacent image):

Template:Center Heavy water reactors and some graphite moderated reactors can use natural uranium, but light water reactors must use low enriched uranium because of the higher neutron absorption of light water. Uranium enrichment removes some of the uranium-238 and increases the proportion of uranium-235. Highly enriched uranium (HEU), which contains an even greater proportion of uranium-235, is sometimes used in the reactors of nuclear submarines, research reactors and nuclear weapons.

If at least one neutron from uranium-235 fission strikes another nucleus and causes it to fission, then the chain reaction will continue. If the reaction continues to sustain itself, it is said to be critical, and the mass of ²³⁵U required to produce the critical condition is said to be a critical mass. A critical chain reaction can be achieved at low concentrations of ²³⁵U if the neutrons from fission are moderated to lower their speed, since the probability for fission with slow neutrons is greater. A fission chain reaction produces intermediate mass fragments which are highly radioactive and produce further energy by their radioactive decay. Some of them produce neutrons, called delayed neutrons, which contribute to the fission chain reaction. The power output of nuclear reactors is adjusted by the location of control rods containing elements that strongly absorb neutrons, e.g., boron, cadmium, or hafnium, in the reactor core. In nuclear bombs, the reaction is uncontrolled and the large amount of energy released creates a nuclear explosion.

Nuclear weapons

The Little Boy gun-type atomic bomb dropped on Hiroshima on August 6, 1945, was made of highly enriched uranium with a large tamper. The nominal spherical critical mass for an untampered ²³⁵U nuclear weapon is Template:Convert,<ref>Template:Cite web</ref> which would form a sphere Template:Convert in diameter. The material must be 85% or more of ²³⁵U and is known as weapons grade uranium, though for a crude and inefficient weapon 20% enrichment is sufficient (called weapon(s)-usable). Even lower enrichment can be used, but this results in the required critical mass rapidly increasing. Use of a large tamper, implosion geometries, trigger tubes, polonium triggers, tritium enhancement, and neutron reflectors can enable a more compact, economical weapon using one-fourth or less of the nominal critical mass, though this would likely only be possible in a country that already had extensive experience in engineering nuclear weapons. Most modern nuclear weapon designs use plutonium-239 as the fissile component of the primary stage;<ref name="FASdesign">Template:Cite book</ref><ref>Template:Cite book</ref> however, HEU (highly enriched uranium, in this case uranium that is 20% or more ²³⁵U) is frequently used in the secondary stage as an ignitor for the fusion fuel.

Source	Average energy released [MeV]<ref name="kayelaby" />
Instantaneously released energy
Kinetic energy of fission fragments	169.1
Kinetic energy of prompt neutrons	Template:FspTemplate:Fsp4.8
Energy carried by prompt γ-rays	Template:FspTemplate:Fsp7.0
Energy from decaying fission products
Energy of β− particles	Template:FspTemplate:Fsp6.5
Energy of delayed γ-rays	Template:FspTemplate:Fsp6.3
Energy released when those prompt neutrons which do not (re)produce fission are captured	Template:FspTemplate:Fsp8.8
Total energy converted into heat in an operating thermal nuclear reactor	202.5 MeV
Energy of anti-neutrinos	Template:FspTemplate:Fsp8.8
Sum	211.3 MeV

Decay

Uranium-235 is an alpha emitter,<ref>Template:NUBASE2020</ref> producing thorium-231. Uranium-235 is the main progenitor of the actinium series, one of the principal actinide decay chains, as it is the longest-lived and sole primordial nuclide (aside from the final end product, lead-207). Beginning with naturally occurring uranium-235, this series includes isotopes of astatine, bismuth, francium, lead, polonium, protactinium, radium, radon, thallium, and thorium, all of which are present in natural uranium sources. The decay proceeds as (only main decay branches shown):

<math chem="">\begin{array}{l}{}\\

\ce{^{235}_{92}U->[\alpha][7.04 \times 10^8 \ \ce y] {^{231}_{90}Th} ->[\beta^-][25.52 \ \ce h] {^{231}_{91}Pa} ->[\alpha][3.27 \times 10^4 \ \ce y] {^{227}_{89}Ac}} \begin{Bmatrix} \ce{->[98.62\% \beta^-][21.772 \ \ce y] {^{227}_{90}Th} ->[\alpha][18.693 \ \ce d]} \\ \ce{->[1.38\% \alpha][21.772 \ \ce y] {^{223}_{87}Fr} ->[\beta^-][22.00 \ \ce{min}]} \end{Bmatrix} \ce{^{223}_{88}Ra ->[\alpha][11.435 \ \ce d] {^{219}_{86}Rn}} \\ \ce{^{219}_{86}Rn ->[\alpha][3.96 \ \ce s] {^{215}_{84}Po} ->[\alpha][1.781 \ \ce{ms}] {^{211}_{82}Pb} ->[\beta^-][36.16 \ \ce{min}] {^{211}_{83}Bi}} \begin{Bmatrix} \ce{->[99.724\% \alpha][2.14 \ \ce{min}] {^{207}_{81}Tl} ->[\beta^-][4.77 \ \ce{min}]} \\ \ce{->[0.276\% \beta^-][2.14 \ \ce{min}] {^{211}_{84}Po} ->[\alpha][0.516 \ \ce s]} \end{Bmatrix} \ce{^{207}_{82}Pb} \end{array}

</math> Or in tabular form, including minor branches:

Nuclide	Decay mode	Half-life (a = years)	Energy released MeV	Decay product
235U	α	7.04×108 a	4.678	231Th
231Th	β−	25.52 h	0.391	231Pa
231Pa	α	3.27×104 a	5.150	227Ac
227Ac	β− 98.62% α 1.38%	21.772 a	0.045 5.042	227Th 223Fr
227Th	α	18.693 d	6.147	223Ra
223Fr	β− 99.994% α 0.006%	22.00 min	1.149 5.561	223Ra 219At
223Ra	α	11.435 d	5.979	219Rn
219At	α 93.6% β− 6.4%	56 s	6.342 1.567	215Bi 219Rn
219Rn	α	3.96 s	6.946	215Po
215Bi	β−	7.6 min	2.171	215Po
215Po	α β− 2.3×10−4%	1.781 ms	7.526 0.715	211Pb 215At
215At	α	37 μs	8.177	211Bi
211Pb	β−	36.16 min	1.366	211Bi
211Bi	α 99.724% β− 0.276%	2.14 min	6.750 0.573	207Tl 211Po
211Po	α	516 ms	7.595	207Pb
207Tl	β−	4.77 min	1.418	207Pb
207Pb	stable

Astrophysical dating

Knowledge of current and theoretical production ratios of uranium-235 to uranium-238 allows radiometric dating, the time since modern uranium nuclei were formed in stellar nucleosynthesis.

The 1957 B2FH landmark paper in astrophysics explained the r-process by which both nuclei form. The authors predicted their relative abundances, and those of their rapidly alpha-chain decaying parent nuclides. Thus they predicted 1.64 as the ²³⁵U/²³⁸U ratio contributed to the interstellar medium by r-process events (supernovae and subsequently discovered kilonovae). This takes billions of years to diminish to their present value of 0.0072 (see natural uranium). They investigate scenarios for historical contribution to the solar nebula, before contribution is cut off at the Sun's formation 4.5 billion years ago. The scenarios are: a single supernova, a finite continuous uniform series of supernovae representing the lifetime of the Milky Way, and an infinite series representing the steady-state universe. From the second scenario, they estimated an age of the Milky Way at around 10 billion years, compared to a modern value of 13.61 billion years. Significantly, at this point the oldest known objects were stellar clusters at 6.5 billion years old.<ref name="l830">Template:Cite journal</ref>

External links

• Table of Nuclides.
• DOE Fundamentals Handbook: Nuclear Physics and Reactor Theory Vol. 1 (Template:Webarchive), Vol. 2 (Template:Webarchive).
• Radionuclide Basics: Uranium—US EPA
• NLM Hazardous Substances Databank – Uranium, Radioactive
• "The Miracle of U-235", Popular Mechanics, January 1941—one of the earliest articles on U-235 for the general public