For a uniform-load bending of a clamped filament, total load $F=wL$ and tip displacement $\delta =w{L}^4/(8B)$ obey Hooke's law in the form $F=k_{\mathrm{eff}}\delta$, with $k_{\mathrm{eff}}=8B/L^3$. This stiffness depends on the specified distributed loading. A concentrated tip force instead gives $3B/L^3$, so equal total forces with different distributions are not interchangeable.

The square of a uniform distribution variable on $(0,1)$ has cumulative distribution function $\sqrt{x}$ and an integrable inverse-square-root probability density function. Reflection replaces $x$ by $1-x$ in that density.

A Steinhaus random variable is uniformly distributed on the complex unit circle. It can be generated as $ϵ\cos \theta +i\delta \sin \theta$ using independent signs $ϵ,\delta$ and an independent uniform angle $\theta \in [0,\pi /2]$. This conditional sign representation transfers Rademacher sum inequalities to random complex phases.

A uniform random variable has a uniform distribution. Independent such variables can supply independent inverse transform sampling; reusing a single variable for two transforms generally creates dependence.

The frequency ${\omega }_d=(GM/R^3{)}^{1/2}=(4\pi G\rho /3{)}^{1/2}$ measures the inverse gravitational timescale of a uniform-density sphere. It is the natural normalization for uniform-density stellar oscillation and the linear restoring or destabilizing accelerations.

When the amplitudes of uniform-density stellar oscillation are finite even polynomials, their highest coefficients close algebraically. With $L=n(2l+n+1)$ and $x={\omega }^2/{\omega }_d^2$, the nonradial coefficient determinant is $x^2+(4-\gamma L/2)x-l(l+1)$. A degree balance gives a necessary frequency relation without solving every lower coefficient or imposing surface conditions.

For the even polynomial family of degree $n\ge 2$, the physical radial squared frequency is $[\gamma n(n+1)/2-4]{\omega }_d^2$. The fundamental $n=2$ mode is stable when $\gamma >4/3$ and marginal at $\gamma =4/3$. At angular degree zero the gradient of the regular solid harmonic vanishes, so the auxiliary displacement amplitude multiplying it is redundant.

Symmetry gives $\Vert (A-z)u\Vert \ge |\mathrm{Im}z|\Vert u\Vert$ when $z$ is nonreal. Closedness makes the range closed; its orthogonal complement is $\ker (A-\overline{z})=0$, so it is also dense and hence surjective. This proves the resolvent estimate and reality of the spectrum. Equality of the adjoint domains is needed in the range argument.

Positivity makes $A-z$ bounded below with dense closed range for every $z<0$, excluding negative spectral values. Conversely if the spectrum is nonnegative, $R=(I+A{)}^{-1}$ has spectrum in $[0,1]$ by the resolvent spectral mapping identity. The numerical-range endpoint approximate-eigenvalue theorem gives $0\le R\le I$, and positive-form Cauchy-Schwarz inequality gives $\Vert Rf{\Vert }^2\le ⟨Rf,f⟩$. For $u=Rf$, $⟨Au,u⟩=⟨Rf,f⟩-\Vert Rf{\Vert }^2\ge 0$.

A charged scalar field coupled to an Abelian gauge field through $D_{\mu }={\partial }_{\mu }-ie{a}_{\mu }$. Under $\varphi \mapsto e^{i\alpha }\varphi$ and $a_{\mu }\mapsto a_{\mu }+e^{-1}{\partial }_{\mu }\alpha$, its gauge covariant derivative transforms with the same phase. The potential determines whether the perturbative spectrum has a massless photon or exhibits the Higgs mechanism.

For a type space $S_n^M(A)$, the basic open set $[\phi ]$ consists of complete types containing the formula $\phi$. These sets are clopen, satisfy $[\phi ]\cap [\psi ]=[\phi \wedge \psi ]$, and distinguish distinct types. The compactness theorem makes this topology compact; it is Hausdorff and has a basis of clopen sets.

If contest rewards and costs add, a fixed deviation's expected payoff depends on each rival's per-contest marginal distributions, rather than on dependence between that rival's efforts across contests. Replacing the conditional independent sampling of two active efforts by another copula with the same conditional marginals therefore preserves every deviation payoff. Consequently it preserves the Nash equilibrium, even when the new joint strategy distribution is different. This explains why unique participation probabilities and bid marginals need not imply a unique full mixed strategy.

On an even ground set $n=2h$, a two-intersecting family has size at most ${\sum }_{j=h+1}^n\left(\genfrac{}{}{0ex}{}{n}{j}\right)$. On an odd ground set $n=2h+1$, the bound is $\left(\genfrac{}{}{0ex}{}{2h}{h+1}\right)+{\sum }_{j=h+2}^n\left(\genfrac{}{}{0ex}{}{n}{j}\right)$. Pair lower levels with complements of upper levels using the intersecting shadow lemma; apply the Erdős-Ko-Rado theorem to the remaining middle level in the odd case.

Fix a member of size $r$. Every other member of a two-intersecting family contains a pair from that fixed member. Counting all $r$-sets containing these pairs gives $|\mathcal{F}|\le \left(\genfrac{}{}{0ex}{}{r}{2}\right)\left(\genfrac{}{}{0ex}{}{n-2}{r-2}\right)$ for a uniform set family.

To pool factor levels in a normal linear model, impose equality of their fitted means while retaining any needed interaction terms. Compare the resulting nested model with the full model using a nested-model F-test. For two cells each of size $m$, pooling their fitted means adds $(m/2)({\overline{Y}}_1-{\overline{Y}}_2{)}^2$ to the residual sum of squares. If pooling two pairs separately within two other-factor levels, there are four restrictions.

The stellar relaxation time is the time on which random gravitational encounters change a star's velocity by an amount comparable to its characteristic random velocity. A weak straight-line encounter at relative speed $u$ and impact parameter $b$ gives a kick $2Gm/(bu)$. Three-dimensional encounter counting gives $d⟨|\Delta \mathbf{v}{|}^2⟩/dt=8\pi G^2{m}^{2}n\log (b_{\max }/b_{\min })/u$. Definitions of relaxation, velocity averaging and system structure alter order-one coefficients; the robust spherical scaling is $t_{\mathrm{rel}}\sim v^3/(G^2{m}^{2}n\log \Lambda )\sim (N/\log N)t_{\mathrm{dyn}}$. Collisionless simulation requirements depend on the duration and permitted fractional relaxation, not a universal minimum particle number.

A collisionless stellar system is one for which discrete gravitational encounters change its distribution negligibly over the time under study, usually $T\ll t_{\mathrm{rel}}$. Stars can orbit and respond collectively to a varying smooth gravitational potential even in this regime; collisionless does not mean force-free or stable against collective gravitational instabilities. Its smooth distribution follows the Collisionless Boltzmann equation.

For a mass $m$ passing at relative speed $u$ and impact parameter $b$, integration of $Gmb/(b^2+u^2{t}^2{)}^{3/2}$ gives the transverse kick $2Gm/(bu)$. Weak deflection requires $b\gg Gm/u^2$, up to the equal-mass order-one factor. This scale supplies a small-impact cutoff for the weak-scattering diffusion approximation, not a physical exclusion of stronger encounters.

In an unsoftened plane with number surface density $n_2$ and relative speed $u$, an encounter strip has area $2udtdb$. Thus the velocity diffusion rate is $8G^2{m}^2{n}_2/u\int db/b^2$, dominated by the small-impact cutoff. Setting this cutoff to $Gm/u^2$ and requiring a change of order $u^2$ gives $t_{\mathrm{rel}}\sim u/(Gm{n}_2)$. With $u=\lambda v$, $n_2\sim N/R^2$ and $v^2\sim GNm/R$, this is of order $\lambda R/v$, independent of $N$ at fixed total mass. The point-particle, zero-thickness limit is singular; fixed softening or nonzero thickness changes it. Numerical coefficients are not controlled by extending weak kicks down to order-one deflections.

For a disk with thickness $z_0$, random relative speeds $u=\lambda v$ and small-impact cutoff $b_0\ll z_0\ll R$, the leading three-dimensional logarithmic encounter term has upper cutoff of order $z_0$. At fixed mass and radius, its number volume density exceeds the spherical density by order $R/z_0$. Hence $t_{\mathrm{disk}}/t_{\mathrm{sphere}}\sim {\lambda }^3(z_0/R)\log (R/b_0)/\log (z_0/b_0)$ when the same cutoff is used for comparison. Different speed-dependent cutoffs must be distinguished in numerical applications. Distant planar encounters contribute a convergent, non-logarithmic correction. This scaling ceases to apply if thickness is comparable to the cutoff.