Neutrons in a sentence

At sea level, the production of neutrons is about 20 neutrons per second per kilogram of material interacting with the cosmic rays (or, about 100-300 neutrons per square meter per second).

Fermi had shown much earlier that neutrons were far more effectively captured by atoms if they were of low energy (so-called "slow" or "thermal" neutrons), because for quantum reasons it made the atoms look like much larger targets to the neutrons.

High KE neutrons are sometimes used for activation, these neutrons are unmoderated and consist of primary fission neutrons.

If enough nuclear fuel is assembled in one place, or if the escaping neutrons are sufficiently contained, then these freshly emitted neutrons outnumber the neutrons that escape from the assembly, and a sustained nuclear chain reaction will take place.

The cadmium cut-off is about 0.5 eV, and neutrons below that level are deemed slow neutrons, distinct from intermediate and fast neutrons.

These delayed neutrons account for about 0.65% of the total neutrons produced in fission, with the remainder (termed " prompt neutrons ") released immediately upon fission.

They are named fission energy or fast neutrons to distinguish them from lower-energy thermal neutrons, and high-energy neutrons produced in cosmic showers or accelerators.

Absorbing more neutrons in a control rod means that there are fewer neutrons available to cause fission, so pushing the control rod deeper into the reactor will reduce its power output, and extracting the control rod will increase it.

After slowing, neutrons may then be absorbed with an isotope that has high affinity for slow neutrons without causing secondary capture radiation, such as lithium-6.

Also because of the short range of the strong binding force, large stable nuclei must contain proportionally more neutrons than do the lightest elements, which are most stable with a 1 to 1 ratio of protons and neutrons.

A moderator increases the power of the reactor by causing the fast neutrons that are released from fission to lose energy and become thermal neutrons.

A portion of these neutrons may later be absorbed by other fissile atoms and trigger further fission events, which release more neutrons, and so on.

As long as the universe was hot enough for protons and neutrons to transform into each other easily, their ratio, determined solely by their relative masses, was about 1 neutron to 7 protons (allowing for some decay of neutrons into protons).

Fast neutrons can be made into thermal neutrons via a process called moderation.

For example, hydrogen -rich materials are often used to shield against neutrons, since ordinary hydrogen both scatters and slows neutrons.

For example, in beta decay a nitrogen -16 atom (7 protons, 9 neutrons) is converted to an oxygen -16 atom (8 protons, 8 neutrons) Not a typical example as it results in a "doubly magic" nucleus within a few seconds of being created.

Free neutrons and protons are less stable than helium nuclei, and the protons and neutrons had a strong energetic reason to form helium-4.

Free neutrons and protons are less stable than helium nuclei, and the protons and neutrons have a strong tendency to form helium-4.

Furthermore, the interaction of energetic photons with protons is similar to the interaction of photons with neutrons citation in spite of the fact that the electric charge structures of protons and neutrons are substantially different.

However, this approach will not work with neutrons, since the absorption of neutrons does not increase straightforwardly with atomic number, as it does with alpha, beta, and gamma radiation.