## Classification of Reactors according to Neutron Flux Spectrum

**neutron energy spectra**. In fact, the

**basic classification**of nuclear reactors is based upon the average energy of the neutrons which cause the bulk of the fissions in the reactor core. From this point of view nuclear reactors are divided into

**two categories**:

**Thermal Reactors.**Almost all of the current reactors which have been built to date use**thermal neutrons**to sustain the chain reaction. These reactors contain neutron moderator that slows neutrons from fission until their kinetic energy is more or less in**thermal equilibrium**with the atoms (E < 1 eV) in the system.**Fast Neutron Reactors.**Fast reactors contains**no neutron moderator**and use**less-moderating primary coolants**, because they use**fast neutrons**(E > 1 keV), to cause fission in their fuel.

**LWR**and a

**sodium-cooled fast breeder reactor**. Note that, the

**fast reactor spectrum**is highly affected by the elastic scattering cross-section of used coolant.

**neutron cross-sections**, that exhibit significant

**energy dependency**. It can be characterized by

**capture-to-fission ratio**, which is

**lower in fast reactors**. There is also a difference in the

**number of neutrons produced per one fission**, which is higher in fast reactors than in thermal reactors. These very important differences are caused primarily by

**differences in neutron fluxes**. Therefore it is very important to know detailed neutron energy distribution in a reactor core.

**Cold Neutrons**(0 eV; 0.025 eV). Neutrons in thermal equilibrium with very cold surroundings such as liquid deuterium. This spectrum is used for neutron scattering experiments.**Thermal Neutrons**. Neutrons in thermal equilibrium with a surrounding medium. Most probable energy at 20°C (68°F) for Maxwellian distribution is**0.025 eV**(~2 km/s). This part of neutron’s energy spectrum constitutes most important part of spectrum**in thermal reactors**.**Epithermal Neutrons**(0.025 eV; 0.4 eV). Neutrons of kinetic energy greater than thermal. Some of reactor designs operates with epithermal neutron’s spectrum. This design allows to reach higher fuel breeding ratio than in thermal reactors.-
**Cadmium Neutrons**(0.4 eV; 0.5 eV). Neutrons of kinetic energy below the**cadmium cut-off**energy. One cadmium isotope,^{113}Cd, absorbs neutrons strongly only if they are below ~0.5 eV (cadmium cut-off energy). **Epicadmium Neutrons**(0.5 eV; 1 eV). Neutrons of kinetic energy above the cadmium cut-off energy. These neutrons are not absorbed by cadmium.**Slow Neutrons**(1 eV; 10 eV).**Resonance Neutrons**(10 eV; 300 eV).**The resonance neutrons**are called resonance for their special bahavior. At resonance energies the cross-sections can reach peaks more than 100x higher as the base value of cross-section. At this energies the neutron capture significantly exceeds a probability of fission. Therefore it is very important (for thermal reactors) to quickly overcome this range of energy and operate the reactor with thermal neutrons resulting in increase of probability of fission.**Intermediate Neutrons**(300 eV; 1 MeV).**Fast Neutrons**(1 MeV; 20 MeV). Neutrons of kinetic energy greater than 1 MeV (~15 000 km/s) are usually named fission neutrons. These neutrons are produced by nuclear processes such as nuclear fission or (ɑ,n) reactions. The fission neutrons have a Maxwell-Boltzmann distribution of energy with a mean energy (for^{235}U fission) 2 MeV. Inside a nuclear reactor the fast neutrons are slowed down to the thermal energies via a process called neutron moderation.**Relativistic Neutrons**(20 MeV; ->)

The reactor physics does not need this fine division of neutron energies. The neutrons can be roughly (for purposes of reactor physics) divided into three energy ranges:

**Thermal neutrons**(0.025 eV – 1 eV).**Resonance neutrons**(1 eV – 1 keV).**Fast neutrons**(1 keV – 10 MeV).

Even most of reactor computing codes use only two neutron energy groups:

**Slow neutrons group**(0.025 eV – 1 keV).**Fast neutrons group**(1 keV – 10 MeV).

## Region of Fast Neutrons

**neutron flux spectrum**in thermal reactors, is the

**region of fast neutrons**. All neutrons produced by fission are born as

**fast neutrons**with high kinetic energy.

At first we have to distinguish between **fast neutrons** and prompt neutrons. The prompt neutrons can be sometimes** incorretly** confused with the fast neutrons. But there is an essential difference between them.** Fast neutrons** are neutrons categorized according to the **kinetic energy**, while** prompt neutrons** are categorized according to the** time of their release**.

Most of the neutrons produced in fission are prompt neutrons. Usually **more than 99 percent** of the fission neutrons are the prompt neutrons, but the exact fraction is dependent on the nuclide to be fissioned and is also dependent on an incident neutron energy (usually increases with energy). For example a fission of ^{235}U by thermal neutron yields **2.43 neutrons**, of which **2.42 neutrons are the prompt neutrons** and 0.01585 neutrons **(0.01585/2.43=0.0065=ß)** are **the delayed neutrons**.

- Prompt neutrons are emitted
**directly from fission**and they are emitted within very short time of about**10**.^{-14}second

- Most of the neutrons produced in fission are prompt neutrons –
**about 99.9%**.

- For example a fission of
^{235}U by thermal neutron yields**2.43 neutrons**, of which 2.42 neutrons are prompt neutrons and 0.01585 neutrons are the delayed neutrons.

- The production of prompt neutrons slightly increase with incident neutron energy.

- Almost all prompt fission neutrons have
**energies between 0.1 MeV and 10 MeV**.

- The mean neutron energy is about
**2 MeV**. The most probable neutron energy is about**0.7 MeV**.

- In reactor design
**the prompt neutron lifetime**(PNL) belongs to key neutron-physical characteristics of reactor core.

- Its value depends especially on the type of the moderator and on the energy of the neutrons causing fission.

- In an infinite reactor (without escape) prompt neutron lifetime is the sum of the
**slowing down time and the diffusion time**.

- In LWRs the
**PNL increases with the fuel burnup**.

- The typical prompt neutron lifetime in thermal reactors is on the order of
**10**second.^{-4}

- The typical prompt neutron lifetime in fast reactors is on the order of
**10**second.^{-7}

Basic features of prompt neutron energy spectra are summarized below:

- The neutrons produced by fission are high energy neutrons.
- Almost all fission neutrons have
**energies between 0.1 MeV and 10 MeV.** - The prompt neutron energy distribution, or spectrum, may be best described by dependence of the fraction of neutrons per MeV on neutron energy.
- The most probable neutron energy is about
**0.7 MeV**.The mean neutron energy is about**2 MeV**. - These values are for thermal fission of
^{235}U, but these values vary only slightly for other nuclides.

Prompt neutron fission spectra evaluation is one of the most interesting aspects of evaluation of actinides. Many experimental and theoretical researches have been carried out for the determination of prompt neutron spectra. There are several representations of prompt fission neutron spectra. Two early models of the prompt fission neutron spectrum, which are still used today, are **the Maxwellian and Watt spectrum**.

The modern spectrum representation of the prompt fission neutron spectrum and average prompt neutron multiplicity is called **the Madland-Nix Spectrum** (Los Alamos Model). This model is based upon the standard nuclear evaporation theory and utilizes an isospin-dependent optical potential for the inverse process of compound nucleus formation in neutron-rich fission fragments.

- The presence of delayed neutrons is perhaps
**most important aspect of the fission process**from the viewpoint of reactor control.

- Delayed neutrons are emitted by neutron rich fission fragments that are called the
**delayed neutron precursors**.

- These precursors usually undergo beta decay but a small fraction of them are excited enough
**to undergo neutron emission.**

- The emission of neutron happens orders
**of magnitude later**compared to the emission of the prompt neutrons.

- About
**240 n-emitters**are known between^{8}He and^{210}Tl, about 75 of them are in the non-fission region.

- In order to simplify reactor kinetic calculations it is suggested
**to group together the precursors**based on their half-lives.

- Therefore delayed neutrons are traditionally represented by
**six delayed neutron groups**.

- Neutrons can be produced also in
**(γ, n) reactions**(especially in reactors with heavy water moderator) and therefore they are usually referred to as**photoneutrons**.**Photoneutrons**are usually treated no differently than regular delayed neutrons in the kinetic calculations.

- The total yield of delayed neutrons per fission, v
_{d}, depends on:- Isotope, that is fissioned.
- Energy of a neutron that induces fission.

- Variation among individual group yields is much greater than variation among group periods.

- In reactor kinetic calculations it is convenient to use relative units usually referred to as
**delayed neutron fraction (DNF)**.

- At the steady state condition of criticality, with k
_{eff}= 1, the delayed neutron fraction is equal to the precursor yield fraction β.

- In LWRs the
**β decreases with fuel burnup**. This is due to isotopic changes in the fuel.

- Delayed neutrons have
**initial energy between 0.3 and 0.9 MeV**with an**average energy of 0.4 MeV**.

- Depending on the
**type of the reactor**, and their**spectrum**, the delayed neutrons may be more (in thermal reactors) or less effective than prompt neutrons (in fast reactors). In order to include this effect into the reactor kinetic calculations**the effective delayed neutron fraction – β**must be defined._{eff}

- The effective delayed neutron fraction is the product of the average delayed neutron fraction and the importance factor
**β**_{eff}= β . I.

- The weighted delayed generation time is given by
**τ = ∑**, therefore the weighted decay constant_{i}τ_{i}. β_{i}/ β = 13.05 s**λ = 1 / τ ≈ 0.08 s**.^{-1}

- The mean generation time with delayed neutrons is about
**~0.1 s**, rather than**~10**as in section Prompt Neutron Lifetime, where the delayed neutrons were omitted.^{-5}

- Their presence completely changes the dynamic time response of a reactor to some reactivity change,
**making it controllable by control systems**such as the control rods.

**very important for the nuclear reactor design**, belong also

**delayed neutron energy spectra**. The energy spectra of the delayed neutrons are the poorest known of all input data required, because it

**very difficult to measure it**.

Depending on the type of the reactor, and their spectrum, the delayed neutrons may be more (in thermal reactors) or less effective than prompt neutrons (in fast reactors). In order to include this effect into the reactor kinetic calculations **the effective delayed neutron fraction – β _{eff} must be defined**.

The vast of the prompt neutrons and even the delayed neutrons are born as fast neutrons (i.e. with kinetic energy higher than > 1 keV). But these two groups of fission neutrons have different energy spectra, therefore they contribute to the fission spectrum differently. Since **more than 99 percent** of the fission neutrons are the prompt neutrons, it is obvious, that they will dominate the entire spectrum.

Therefore the fast neutron spectrum can be described by following points:

- Almost all fission neutrons have
**energies between 0.1 MeV and 10 MeV**. - The mean neutron energy is about
**2 MeV**. - The most probable neutron energy is about
**0.7 MeV**.

The fast neutron spectrum can be approximated by the following (normalized to one) distribution:

The neutrons released during fission with an average energy of**2 MeV**in a reactor on average undergo a

**number of collisions**(elastic or inelastic) before they are absorbed. As a result of these collisions

**they lose energy**, so that the

**reactor spectrum is not identical to the fission spectrum**, it is always

**‘softer’**than the fission spectrum. The fact is that the fission spectrum is the part of the reactor spectrum.

## Thermal vs. Fast Reactors

**reactor design**. The previous figure illustrates the difference in

**neutron flux spectra between a thermal reactor and a fast breeder reactor**. Note that, the neutron spectra in fast reactors also vary significantly with a given reactor coolant. For example, gas-cooled reactors have significantly harder neutron spectra than that of neutron spectra in sodium-cooled reactors. The main differences in the curve shapes may be attributed to the neutron moderation or slowing down effects.

## Intermediate Energy Region

**insignificant number of neutrons**that can reach the thermal energies or the intermediate energies. On the other hand,

**in thermal reactors**, neutrons have to be moderated in order to profit from the larger cross-sections at lower energies. In these reactors, the neutrons are predominantly absorbed only when they are in kinetic equilibrium with the thermal movement of the surrounding atomic nuclei.

**Between the fast region and the thermal region** there is an **intermediate energy region (1 eV to 0.1 MeV)**. For this region the** 1/E dependency** is typical. That is, if the energy (E) is halved, the flux **Ф(E) **doubles. This 1/E dependence is caused by the the nature of the slowing down process. In this region** Σ _{s}(E)** varies only little. The elastic scattering remove a

**constant fraction**of the neutron energy per collision (see logarithmic energy decrement), independent of energy. Therefore the neutron loses

**larger amounts of energy**per collision

**at higher energies**than at lower energies. The fact that the neutrons lose a constant fraction of kinetic energy per collision causes the energy dependent neutron flux to tend to “pile up” at lower energies.

## Thermal Region

**thermal region**the neutrons achieve a thermal equilibrium with the atoms of the moderator material (in

the idealized situation where no absorption is present). That is the neutrons behave as a strongly diluted gas in thermal equilibrium. These neutrons do not all have the same energy, there is a distribution of energies, usually known as

**the Maxwell-Boltzmann distribution**: in which

**k**is the

**Boltzmann constant**(k = 8.52⋅10

^{-5}eV/K). For the thermal neutron flux density it thus holds that: in which n

_{0}is the total thermal neutron density.

The **most probable energy** (for which the spectrum is maximum) is E = kT. At room temperature this is **0.025 eV**. The velocity corresponding with this energy is 2200 m/s. This energy is of particular importance since reference data, such as** nuclear cross-sections**, are tabulated for a neutron velocity of 2200 m/s.

At a reactor temperature of 320°C (593 K), a value characteristic for PWRs, the most probable velocity is 3100 m/s and the corresponding energy is 0.051 eV.

But this distribution only holds for **complete thermal equilibrium**. Unfortunately, in a nuclear reactor, some absorption will always be present and this equilibrium will never be complete. As a result of 1/v behaviour, low energy neutrons are absorbed preferentially, which leads to a shift of the spectrum to higher energies.

On the other hand, the **neutron leakage** has an** opposite effect**. With decreasing energy the **diffusion coefficient D** decreases as a result of the increasing cross-sections, therefore the neutron leakage preferentially removes neutrons with higher energies. This effect strongly depends on the size of the multiplying system, but in most cases it is much less important than the presence of absorption.

**Nuclear and Reactor Physics:**

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**Advanced Reactor Physics:**

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