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A spherical three-momentum ultraviolet cutoff givesFor $m>0$ and $\Lambda \gg m$, the asymptotic expansion isIn particular, the leading ultraviolet divergence is quartic. For $m=0$, $\mathcal{E}={\Lambda }^4/(16{\pi }^2)$ exactly.

Write $\phi =⟨\psi ⟩$. Under the proposed identification, the scalar potential from a field-dependent momentum cutoff is $V_{\mathrm{ind}}(\phi )=\mathcal{E}(|\phi |)$. It is even and nonnegative, and its derivative with respect to $|\phi |$ is $|\phi {|}^2\sqrt{{\phi }^2+m^2}/(4{\pi }^2)>0$ away from zero. Consequently its only global minimum is at $\phi =0$: this contribution alone does not cause spontaneous symmetry breaking. At large $|\phi |$ it grows quartically. At small $|\phi |$ with fixed positive $m$, however,Thus the quartic sketch is an asymptotic shape, not the exact small-field behavior for a massive original field. Identifying a regulator with a new field is an additional modeling prescription; an actual effective potential also depends on the new field's dynamics and any other allowed terms.

Goldstone's theorem states that a spontaneously broken continuous internal global symmetry in field theory of a local relativistic quantum field theory produces massless Goldstone bosons. For a Lorentz invariance vacuum breaking $G$ to its stabilizer $H$, there are $\dim G-\dim H$ independent symmetry-required massless directions. Additional accidentally massless modes are possible. A gauge redundancy does not obey this physical-state counting, and nonrelativistic systems need not have one independent mode per broken generator.

For the classical proof, consider real scalar fields ${\varphi }_i$ with a positive canonical kinetic term and an invariant smooth scalar potential $V$. An infinitesimal generator $T^a$ satisfiesLet $v$ be a stationary vacuum and differentiate this identity with respect to ${\varphi }_j$. At $v$, the term proportional to ${\partial }_{i}V$ vanishes, leavingThe Hessian matrix ${\mathsf{M}}^2$ is the scalar mass matrix. An unbroken generator has $T^{a}v=0$; broken generators span the tangent space of the vacuum manifold $G/H$. Each independent nonzero tangent vector is a zero eigenvector of ${\mathsf{M}}^2$. The quadratic Euler-Lagrange equations in these directions are $\square {\pi }^a=0$, giving the massless dispersion relation ${\omega }^2={\mathbf{p}}^2$. This proves the classical result and explains why the Goldstone bosons describe motion along the degenerate minima rather than against a restoring curvature.

Assume ${\mu }^2,\lambda >0$. At zero source, the vacuum manifold is the sphere of radius $v_0=\mu /\sqrt{\lambda }$. The source tilts the scalar potential by $-ϵ{\varphi }_1$. Its force should be small compared with the radial restoring-force scale ${\mu }^2{v}_0$, so a useful quantitative condition isFor nonzero $ϵ$, the exact global symmetry in field theory of the Lagrangian is $O(n-1)$, rotating ${\varphi }_2,\dots ,{\varphi }_n$. The global vacuum aligns with the source:This vacuum preserves the entire remaining $O(n-1)$ symmetry. There is therefore no exact Goldstone boson for $ϵ\ne 0$. Expanding the scalar potential to quadratic order givesThus there are $n-1$ degenerate light pseudo-Goldstone bosons and one heavy radial scalar. The small-source condition makes their squared masses parametrically smaller than the radial squared mass. Sending $ϵ$ to zero restores the original massless modes.

In an effective field theory, higher-power terms in an inflaton scalar potential can be important when $\varphi /M_{\mathrm{Pl}}$ is large, even if $V/M_{\mathrm{Pl}}^4$ is small. An assumed simple monomial inflation potential over such a field range needs a symmetry or ultraviolet completion controlling these operators and radiative corrections. A large field value alone does not establish Planckian energy density or invalidate every possible completion.

The Polonyi model uses one chiral superfield, a canonical Kähler potential and a linear superpotential to study supersymmetry breaking. In a global theory, $W={\mu }^2\Phi +W_0$ with $\mu \ne 0$ gives a constant nonzero auxiliary field and scalar potential $V=|\mu {|}^4$, leaving the scalar direction flat at this level.

In supergravity, the constant $W_0$ matters and the relevant condition is the vanishing of the Kähler covariant derivative of a superpotential, rather than its ordinary derivative. Consequently, a linear superpotential does not break supersymmetry for every parameter choice. An appropriate constant can instead give a stable zero-energy vacuum with a nonzero supergravity auxiliary field. This simple model separates the questions of vacuum energy, scalar stabilization and supersymmetry breaking.

A potential for a conservative vector field $X$ is a function with scalar values $\Phi$ whose gradient is $X$. Potentials differ by a constant on each connected component. The fundamental theorem for line integrals gives ${\int }_{\gamma }X\cdot d\mathbf{x}=\Phi (\gamma (1))-\Phi (\gamma (0))$. In mechanics a conservative force is conventionally written $-\nabla V$, so its potential energy is $V=-\Phi$. This spatial potential differs from the scalar potential $V(\varphi )$ that denotes the derivative-free energy density of a scalar field.

In a canonical Wess–Zumino model with cubic superpotential $g{\Phi }^3/3$, auxiliary elimination gives a complex-scalar quartic interaction with two legs of each field type. With all momenta incoming and the displayed coefficient, its Feynman rule is $-i(2!2!)|g{|}^2$. For $\phi =(A+iB)/\sqrt{2}$, the same quartic scalar potential is $|g{|}^2(A^2+B^2{)}^2/4$, with real-field rules $-6i|g{|}^2$ for four identical legs and $-2i|g{|}^2$ for two of each. Factorials depend on how the coefficient is defined, not on a new physical coupling.

For a free electromagnetic field with suitable boundary conditions, combine Coulomb gauge ${\partial }_i{A}_i=0$ with $A_0=0$. Gauss's law makes the second condition consistent in the source-free problem. The remaining field operator is spatially transverse and describes the two radiative photon polarizations. A constrained scalar potential must be restored when charges are present.

A radiative correction is a quantum correction beyond the classical or tree approximation, represented in perturbative quantum field theory by Feynman diagrams of positive loop order. Such corrections can alter a scalar potential and its derivatives; symmetries and renormalization constrain which changes are allowed.

Radius stabilization fixes the size of a compactification dynamically rather than choosing it as an undetermined parameter. If the four-dimensional low-energy effective action contains a radion $R$ with positive kinetic coefficient $Z(R)$ and scalar potential $V(R)$, a stable radius $R_0$ requires $V^{\prime }(R_0)=0$ and $m_R^2=V^{\prime \prime }(R_0)/Z(R_0)>0$. This matters for the hierarchy problem: the volume or warp factor explains a hierarchy only if a consistent dynamics selects and maintains the required geometry.

Reheating transfers the inflaton energy into other particles after cosmic inflation, eventually establishing a hot thermal bath. It requires interactions in addition to a background scalar potential. The duration and averaged equation-of-state parameter of reheating affect the number of e-folds between a chosen scale's horizon exit and the end of inflation.

The reheating temperature characterizes the thermal radiation bath after a nonthermal component transfers its energy to other particles and those particles reach thermal equilibrium. Use natural units and the reduced Planck mass $M=(8\pi G{)}^{-1/2}$. In the sudden decay of a dominant nonrelativistic relic, decay rate $\Gamma$ and the Friedmann equation give ${\rho }_R\simeq 3M^2{\Gamma }^2$ at $H\simeq \Gamma$. Equating this with equilibrium radiation energy density givesHere $g_{\ast ,\rho }$ counts the effective relativistic energy degrees of freedom, so the formula can be implicit when the particle content changes with temperature. For example, increasing $\Gamma$ by a factor four doubles this estimate at fixed $g_{\ast ,\rho }$.

The residual bath just before decay can be much colder, while gradual reheating can temporarily produce a maximum bath temperature above the eventual radiation-domination value. Prompt energy transfer is also distinct from prompt thermalization. A scalar scalar potential alone therefore does not fix $T_R$ without interactions and a transfer history.^[ref]

A homogeneous canonical scalar field contributes energy density $\rho ={\dot{\phi }}^2/2+V$ and pressure $P={\dot{\phi }}^2/2-V$. When it is the only source in a spatially flat FLRW metric, the Friedmann equation is $3M_{\mathrm{Pl}}^2{H}^2=\rho$, and its evolution follows the scalar field equation of motion. Positive energy density implies $w\ge -1$ because $\rho +P={\dot{\phi }}^2\ge 0$, even if the scalar potential is negative.

For a canonical real scalar field with metric signature $(-,+,+,+)$ and scalar potential $V$, variation of its minimally coupled action gives the displayed equation. A homogeneous field in an FLRW metric therefore obeys $\ddot{\phi }+3H\dot{\phi }+V^{\prime }(\phi )=0$ in natural units. Its energy density is ${\dot{\phi }}^2/2+V$ and its pressure is ${\dot{\phi }}^2/2-V$, which satisfy the cosmological continuity equation.

For real scalar fields with canonically normalized quadratic kinetic terms, the tree-level scalar mass matrix is the Hessian matrix of the scalar potential at a stationary vacuum:Its eigenvalues are squared masses in units $c=\hslash =1$. A negative eigenvalue is a local instability of that candidate vacuum.

The kinetic normalization is essential. More generally, expand about ${\varphi }_0$ withwhere $H$ is the potential Hessian matrix and $K$ is a real symmetric positive-definite matrix. A mode $\eta =v{e}^{-ip\cdot x}$ obeys the generalized eigenvalue problemEquivalently, canonical field normalization gives the symmetric squared-mass matrix $K^{-1/2}H{K}^{-1/2}$. For one field with kinetic coefficient $Z>0$ and quadratic potential $m_0^2{\varphi }^2/2$, the physical squared mass is $m_0^2/Z$.

Broken continuous global-symmetry directions are zero vectors of the potential Hessian matrix, producing Goldstone bosons when the kinetic form is nonsingular. A Higgs mechanism changes which scalar modes remain independent physical particles; explicit symmetry breaking can lift a zero mass. Thus both the potential and kinetic structure are needed to read a physical spectrum.

A scalar potential is the derivative-free energy density $V(\varphi )$ of a scalar field. Its derivative supplies the force term in the field equation, and its local minima describe candidate vacuum field values.

If a free real scalar field's three-momentum ultraviolet cutoff is identified with the absolute vacuum expectation value of another scalar field, the displayed scalar potential is even and has its unique global minimum at zero. It grows as ${\phi }^4/(16{\pi }^2)$ for $|\phi |\gg m$, but as $m|\phi {|}^3/(12{\pi }^2)$ for $|\phi |\ll m$ with $m>0$. The positive derivative with respect to $|\phi |$ proves that this contribution alone does not produce spontaneous symmetry breaking. This cutoff identification is a model assumption, distinct from deriving a complete effective potential for a dynamical field.

An unbroken subgroup $H$ must fix the vacuum expectation value $v$ of a scalar field in a group representation $V$. Thus a nonzero such $v$ exists exactly when $V^H\ne \{0\}$. For a compact group, complete reducibility of compact-group representations identifies this fixed vector subspace with the sum of the trivial representations in the restriction of a representation $V{|}_H$. Every $v\in V^H$ has $H\subseteq \mathrm{Stab}(v)$; equality requires a separate stabilizer calculation. The criterion neither determines the full unbroken group nor guarantees that a given scalar potential has its minimum at that direction.

The scalar potential $V(\Phi )=\lambda ({\Phi }^T\Phi -v^2{)}^2/4$, with $\lambda >0$, is invariant under the SO(3) group. For $v>0$, its vacuum manifold is a sphere. Canonical scalar normalization gives radial mass squared $2\lambda v^2$.

A Yang-Mills theory with gauge group $SO(3)$ and a real three-component scalar field in its defining vector representation. With a symmetry-breaking scalar potential, a nonzero vector vacuum leaves its $SO(2)$ stabilizer subgroup unbroken. The two transverse internal directions produce massive gauge bosons.