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With a momentum-independent allowed nuclear matrix element, negligible nuclear recoil and negligible neutrino mass, the electron spectrum in natural units is $d\Gamma /dp=CF(Z,E)p^2(E_0-E{)}^2$, where $E=\sqrt{p^2+m_e^2}$. Transforming to an energy spectrum requires the Jacobian determinant $dp/dE=E/p$.

This effective baryon mass model adds a colour-magnetic spin-spin interaction to a sum of constituent quark masses. The common coefficient $A^{\prime }$ absorbs a spatial contact density, colour factors, and the strong coupling. $A^{\prime }$ has dimensions of energy cubed in natural units. A shared coefficient is an approximation because different flavour configurations can have different spatial wavefunctions.

Black-body radiation is the electromagnetic radiation in thermal equilibrium with an ideal blackbody. It can be described as a photon gas: a cavity whose walls are all at the same temperature contains radiation with the universal Planck's law spectrum. A small opening in such a cavity approximates a blackbody emitter because incoming radiation undergoes repeated absorption inside. The radiation's equilibrium spectrum depends on temperature, rather than the wall material. ^[ref]

There are three useful quantities to keep distinct: directional spectral radiance $B_{\nu }$ or $B_{\lambda }$, total energy density $u$ in the cavity, and outward radiant exitance $j^{\ast }$ from its opening. Planck's law supplies the first; integrals over frequency and directions supply the others. For isotropy, every direction has the same $B_{\nu }$, so the full $4\pi$ solid angle givesHere $\hslash =h/(2\pi )$ is the reduced Planck constant, and the radiation constant is $a_{\mathrm{rad}}\approx 7.565733250\times 10^{-16}\mathrm{J}{\mathrm{m}}^{-3}{\mathrm{K}}^{-4}$. The explicit Boltzmann constant makes this an SI formula; adopting natural units with $k_B=1$ recovers $u={\pi }^2{T}^4/(15{\hslash }^3{c}^3)$.

For a short integral outline, substitute $x=h\nu /(k_{B}T)$ and useThe expansion is a geometric series with nonnegative terms; repeated integration by parts evaluates each integral, and $\zeta (4)={\pi }^4/90$ is a value of the Riemann zeta function. This gives the coefficient above.

The photon gas also exerts radiation pressure, $p=u/3$. The factor $1/3$ comes from the angular average of the squared directional component of photon momentum, $⟨{\cos }^2\theta ⟩=1/3$. The thermodynamic derivation of blackbody radiation pressure gives the same result. In contrast, outgoing power involves one projected-direction factor over an outward hemisphere, yielding radiant exitanceThis is the Stefan–Boltzmann law with unit emissivity; $\sigma$ is the Stefan-Boltzmann constant. The factor $\pi$ follows from Lambert's cosine law, rather than the $4\pi$ full-sphere factor used for energy density.

For example, an ideal $6000\mathrm{K}$ cavity has $u\approx 0.980519\mathrm{J}{\mathrm{m}}^{-3}$, radiation pressure $p\approx 0.326840\mathrm{Pa}$, and outward radiant exitance $j^{\ast }\approx 7.34881\times 10^7\mathrm{W}{\mathrm{m}}^{-2}$. A stipulated $3000\mathrm{K}$ cavity has one-sixteenth each value because all three scale as $T^4$. These describe stored energy, mechanical pressure, and outgoing power per area, respectively. In a closed equilibrium cavity, equal opposing radiation balances the directional power flow even though $u$ and $p$ are nonzero.

The usefulness of black-body radiation is this common reference: Planck's law, Wien's displacement law, and the Stefan–Boltzmann law consistently connect spectral measurements, temperature, and total emission. The three illustrative curves in Planck's law are ideal equilibrium spectra; applying them to a material requires considering its emissivity and whether thermal equilibrium is a suitable approximation.

Boltzmann suppression is the exponential reduction of an equilibrium population when creating it costs energy much greater than the temperature. For a nonrelativistic species with negligible chemical potential, the leading factor is $e^{-m/T}$, multiplied by its momentum phase-space volume. It concerns the equilibrium abundance; freeze-out can preserve a larger population than the instantaneous equilibrium value at later times.

Here natural units set the Boltzmann constant and the speed of light to one, so the mass $m$ denotes its rest-energy and $T$ has energy units. In ordinary units the exponential function has argument $-m{c}^2/(k_{B}T)$.

A nonrelativistic species with $g$ states and negligible chemical potential has equilibrium density $g(mT/(2\pi ){)}^{3/2}{e}^{-m/T}$. If particle-antiparticle annihilation maintains equilibrium after the species becomes massive, its eventual freeze-out population can be much smaller than a relativistically decoupled population. The nonrelativistic annihilation rate and any asymmetry determine the final abundance.

Here natural units set the Boltzmann constant and the speed of light to one, so the mass $m$ denotes its rest-energy and $T$ has energy units. In ordinary units the exponential function has argument $-m{c}^2/(k_{B}T)$.

For an isolated particle resonance of spin $J_R$, the Breit-Wigner approximation relates a production-and-decay cross section to its partial decay widths. In natural units, $p_i$ is either incident particle's momentum magnitude in the centre-of-momentum frame, $g=(2J_R+1)/[(2J_a+1)(2J_b+1)]$ for unpolarized incident particles, and $\Gamma$ is the total width. The formula assumes the stated spin counting and neglects nonresonant backgrounds and their interference. Multiplication by $(\hslash c{)}^2$ converts an inverse-squared-energy cross section to area when momenta are expressed in energy units.

The canonical stress-energy tensor is the Noether current associated with translation symmetry. For a Lagrangian density with no explicit coordinate dependence,

The Euler-Lagrange field equations imply ${\partial }_{\mu }{T}^{\mu }{}_{\nu }=0$. Thus $T^0{}_{\nu }$ are conserved densities and $T^i{}_{\nu }$ their fluxes; integrated charges are conserved when the boundary flux vanishes. For a real scalar field with $\mathcal{L}=\frac{1}{2}(\partial \Phi {)}^2-\frac{1}{2}{m}^2{\Phi }^2$, the energy density is $T^{00}=\frac{1}{2}{\dot{\Phi }}^2+\frac{1}{2}|\nabla \Phi {|}^2+\frac{1}{2}{m}^2{\Phi }^2$ in natural units. The general canonical stress-energy tensor need not be symmetric. ^[ref]

For a massless incident neutrino and a stationary target electron, the invariant squared center-of-mass energy is $s=m_e^2+2m_e{E}_{\nu }$ in natural units. Production of a charged lepton of mass $m_{\ell }$ and a massless neutrino requires $s\ge m_{\ell }^2$, giving the displayed threshold. For the electron flavour the threshold is zero; for heavier charged leptons it is enhanced by the small stationary-target mass.

A positively curved pressureless matter universe with zero cosmological constant has the cycloid parametrization displayed above. In natural units, if the Friedmann equation is ${\dot{a}}^2=C/a-k$ with $C,k>0$, then $A=C/(2k)$ and $u=\sqrt{k}\tau$ for conformal time measured from the Big Bang. Substituting in $a^{\prime 2}=Ca-k{a}^2$ verifies the scale factor; integrating $dt=ad\tau$ gives cosmic time. The universe reaches maximum size at $u=\pi$ and recollapses into a Big Crunch at $u=2\pi$.

Cosmic microwave background diffusion damping, or Silk damping, damps the photon-baryon acoustic oscillator on small scales because Thomson scattering gives photons a finite mean free path. Repeated scatterings mix hotter and colder regions. Departures from perfect tight coupling also appear as photon-baryon velocity slip and a photon quadrupole, producing heat-conduction and shear-viscosity damping.

In natural units, the positive conformal scattering rate is ${\Gamma }_T=a{n}_e{\sigma }_T$, with proper free-electron number density $n_e$. A random-walk estimate gives squared comoving diffusion distance of order $\int d\eta /{\Gamma }_T$. More precisely, the leading polarization-inclusive tight-coupling amplitude containswhere $R=3{\rho }_b/(4{\rho }_{\gamma })$ is the baryon loading parameter. The corresponding power spectrum suppression is $e^{-2k^2/k_D^2}$. The approximation applies while the expansion in scattering time is controlled; it cannot be extended through a transparent universe by simply integrating $1/{\Gamma }_T$ indefinitely.^[ref]

Diffusion accumulates before last scattering and becomes especially important as the free-electron population falls. The finite width of the cosmological visibility function can also average oscillating line-of-sight sources; that averaging is a distinct mechanism acting in the same epoch. Both effects help shape the small-angular-scale damping tail, whose scale probes the ionization and baryon history.

In natural units, conservation of the stress-energy tensor for a homogeneous perfect fluid in an FLRW metric gives the displayed equation for its energy density and pressure. It is equivalent to $d(\rho a^3)=-Pd(a^3)$. For a constant equation-of-state parameter $w=P/\rho$, separation gives $\rho \propto a^{-3(1+w)}$. If $\rho$ instead denotes mass density, the pressure term is $P/c^2$.

This is local stress-energy conservation; it does not in general define a globally conserved total energy for an expanding universe. The adiabatic work in a comoving volume makes this distinction explicit.

Use natural units and a positive nuclear binding energy ${\epsilon }_D=m_n+m_p-m_D$. Chemical equilibrium of $n+p\leftrightarrow D+\gamma$ requires ${\mu }_D={\mu }_n+{\mu }_p$. The nonrelativistic Maxwell--Boltzmann number density givesHere $g_D=3$ and $g_n=g_p=2$ count the spin states. Taking $m_n\simeq m_p\simeq m_N$ and $m_D\simeq 2m_N$, then writing $X_i=n_i/n_B$, $n_B=\eta n_{\gamma }$ and using the photon number density yields the displayed abundance. The coefficient is approximately $8.14$. Omitting the spin-state ratio $3/4$ gives the rougher prefactor $16\zeta (3)/\sqrt{\pi }$. A convention $B=m_D-m_n-m_p<0$ instead writes the exponential as $e^{-B/T}$. The small baryon-to-photon ratio suppresses stable deuterium until the temperature is well below the binding scale, producing the deuterium bottleneck.

For a free target electron at rest, $e^{-}{e}^{-}\to e^{-}{e}^{-}{e}^{-}{e}^{+}$ has threshold invariant mass $4m_e$. In natural units, $s=2m_e^2+2m_e{E}_{\mathrm{incident}}$ gives incident total energy $7m_e$, or incident kinetic energy $6m_e$. Atomic binding and recoil of the rest of an atom are excluded by this free-target model. This threshold differs from photon-induced pair production.

For an exactly massless minimally coupled scalar field on flat-slicing de Sitter spacetime with constant $H$, use natural units and neglect its metric backreaction. With $a=-1/(H\tau )$ and the Bunch-Davies vacuum, its canonical mode isWith power spectrum convention $⟨\delta {\varphi }_{\mathbf{k}}\delta {\varphi }_{{\mathbf{k}}^{\prime }}⟩=(2\pi {)}^3{\delta }^3(\mathbf{k}+{\mathbf{k}}^{\prime })P_{\delta \varphi }(k,\tau )$, taking the squared mode amplitude givesThe constant part is the frozen contribution to a de Sitter scalar spectrum; the remaining part is the subhorizon vacuum contribution to a de Sitter scalar spectrum. A merely light but nonzero mass changes the exact mode equation, so the displayed massless solution is then an approximation rather than an exact identity. Nonminimal curvature coupling also changes it.

The massless infinite-volume two-point correlation function has an infrared divergence. A finite-volume or finite-duration infrared prescription is needed, and coincident products require ultraviolet regulation or smearing. A finite spectrum at each fixed nonzero $k$ does not by itself make the all-mode equal-position integral finite.

The Euler-Lagrange field equation implements the principle of stationary action for a Lagrangian density depending on scalar fields and their first derivatives. For a single scalar field $\Phi$,

Vary $S=\int d^{4}x\mathcal{L}$. Integration by parts transfers the derivative from $\delta \Phi$ to $\partial \mathcal{L}/\partial ({\partial }_{\mu }\Phi )$. The boundary term vanishes for variations supported away from the boundary; arbitrary interior variations then force the displayed coefficient to vanish. For $\mathcal{L}=\frac{1}{2}{\partial }_{\mu }\Phi {\partial }^{\mu }\Phi -\frac{1}{2}{m}^2{\Phi }^2$, the result is the Klein-Gordon equation $({\partial }_{\mu }{\partial }^{\mu }+m^2)\Phi =0$, using natural units and Minkowski metric signature $(+---)$. ^[ref]

In a spatially flat universe dominated by a homogeneous canonical scalar field, use natural units and reduced Planck mass $M$. For $\lambda >0$, ${\varphi }_0>0$ and $t>0$, takeThis is an exact solution for a particular scalar potential, not for an arbitrary prescribed potential. The identities $\dot{H}=-{\dot{\varphi }}^2/(2M^2)$ and $V=3M^2{H}^2-{\dot{\varphi }}^2/2$ reconstruct it asTo check the reconstruction, $\dot{\varphi }=2\lambda {\varphi }_0/\sinh (2\lambda t)$ and $\sinh (\varphi /{\varphi }_0)=-1/\sinh (2\lambda t)$. The scalar equation then follows from the Friedmann equation and energy conservation where $\dot{\varphi }\ne 0$.

For $2/3<\beta <2$, the potential is positive and expansion begins as a decelerating power law $a\propto t^{\beta /2}$. At late times $H\to \lambda \beta$ and expansion becomes exponential. More precisely ${ϵ}_H=-\dot{H}/H^2=(2/\beta ){\mathrm{sech}}^2(2\lambda t)$ decreases through one. This illustrates entry into late accelerated expansion rather than a graceful exit from inflation.

Use natural units, the unreduced Planck mass $m_P=G^{-1/2}$, $V_0>0$ and $c\ne 0$. In a flat universe dominated by a canonical inflaton, $\varphi =(2m_P/c)\log (\beta t)$ and $a\propto t^p$ solve the inflaton equation of motion and Friedmann equation exactly when $p=16\pi /c^2$ and ${\beta }^2=V_0{c}^2/[2m_P^2(3p-1)]$. The positive-potential scaling solution requires $p>1/3$, while cosmic inflation requires $p>1$. Its constant equation-of-state parameter is $w=-1+2/(3p)$. In terms of the reduced Planck mass $M=m_P/\sqrt{8\pi }$, the exponential slope is $\lambda =c/\sqrt{8\pi }$ and the same exponent is $p=2/{\lambda }^2$.

In rationalized natural units, the fine-structure constant is $\alpha =e^2/(4\pi )$. It measures the electromagnetic interaction strength. Its use in a specified perturbative calculation requires a consistent coupling and renormalization scale convention.

Work in natural units with $c=1$, neglect the electron mass, and put the initial proton at rest with mass $M$. Let $k$ and $k^{\prime }$ be the initial and final electron four-momenta, $q=k-k^{\prime }$, and $Q^2=-q^2>0$. Define the laboratory energy transfer ${\nu }_{\mathrm{lab}}=E-E^{\prime }=P\cdot q/M$. This ${\nu }_{\mathrm{lab}}$ has units of energy; the invariant $P\cdot q$ has units of energy squared. The Bjorken scaling variable and the final hadron invariant mass obeyThese follow by squaring $k-k^{\prime }$ and $P+q$, using $k^2=k^{\prime 2}=0$ and $P=(M,0)$. Solving the Bjorken x definition gives the outgoing energy and then the scattering angle:Alternatively, substituting $Q^2=4E{E}^{\prime }{\sin }^2(\theta /2)$ before solving gives $E^{\prime }=E/[1+2E{\sin }^2(\theta /2)/(Mx)]$. A chosen $x,E,Q^2$ must satisfy $E^{\prime }>0$ and $0\le {\sin }^2(\theta /2)\le 1$. In addition, $W$ must exceed the lightest allowed inelastic hadron threshold; positive $W^2$ alone is insufficient.

For an original numerical example, take $M=0.938\mathrm{GeV}$, $x=0.3$, $E=15\mathrm{GeV}$ and $Q^2=3{\mathrm{GeV}}^2$. Then ${\nu }_{\mathrm{lab}}\simeq 5.330\mathrm{GeV}$, $E^{\prime }\simeq 9.670\mathrm{GeV}$, $\theta \simeq 8.25^{\circ }$, and $W\simeq 2.807\mathrm{GeV}$. Varying $2\le Q^2/{\mathrm{GeV}}^2\le 5$ and $10\le E/\mathrm{GeV}\le 20$ at this same Bjorken x keeps every setting physical and gives $W^2>5.54{\mathrm{GeV}}^2$, above the proton-pion threshold and the stricter chosen continuum selection $W>2\mathrm{GeV}$. These are calculated settings, not historical measurements.

The four-momentum operator collects the generators of spacetime translations in quantum field theory. With physical speed of light $c$,For the mostly-minus Minkowski metric,All components of $P^{\mu }$ therefore have units of momentum; $P\cdot a$ has units of action. The natural units convention $c=1$ gives the common abbreviation $P^{\mu }=(H,\mathbf{P})$.

A simultaneous momentum eigenstate satisfies $P^{\mu }|p⟩=p^{\mu }|p⟩$, where $p^{\mu }=(E/c,\mathbf{p})$ is its four-momentum. On a one-particle state of rest mass $m$, the mass-shell relation is $p_{\mu }{p}^{\mu }=m^2{c}^2$.

In a translation-invariant theory the four translation generators commute. A translation-invariant vacuum state has zero spatial momentum; after subtracting the additive vacuum energy, it also has zero Hamiltonian eigenvalue. This fixes the vacuum origin of the four-momentum spectrum.