To find an input of a permutation whose output lies in a known $K$-element subset, compute the output, apply its marked-state phase oracle, and use uncomputation. A modular-addition quantum oracle costs two forward queries per marked reflection, because modular-oracle inversion by negation supplies its inverse. Amplitude amplification then uses $O(\sqrt{N/K})$ queries for fixed success probability. Positive-square outputs have $K=\lfloor \sqrt{N-1}\rfloor$ and hence query cost $O(N^{1/4})$.

This mapping torus fibers over the circle with fiber $T^{n-1}$ and inversion as monodromy. The Wang sequence computes its additive cohomology. Coordinate projections to the Klein bottle expose its mod-two cup products.

A mobile-lid mode of planetary evolution in which coherent pieces of the lithosphere move, form at spreading regions and can recycle through subduction. Slab pull, ridge push and mantle flow compete with deformation resistance. It affects heat transport, volcanism, earthquakes and the carbonate-silicate cycle. It is not guaranteed solely by an exoplanet's mass.

The direct channel combines the two incoming four-momentum vectors. A one-particle pole in this channel has the intermediate particle's squared mass equal to $s$. Imaginary rapidity differences can satisfy this mass relation for a bound state even though there is no pole at real physical scattering rapidity.

With a specified ordering of external legs, this crossed channel carries the difference between an incoming and an outgoing energy-momentum vector. A one-particle exchange pole requires that difference to be on the exchanged particle's mass shell. Ordered amplitudes in one spatial dimension can label the crossed invariant using the difference of the two rapidity-parameterized external momenta; the external-leg convention fixes which crossed invariant is named $t$.

A plane-parallel magnetostatic equilibrium with constant downward gravitational acceleration $g$, horizontal magnetic field, constant isothermal sound speed $c_s$, and constant Alfvén speed $v_a$ hasIndeed the magnetohydrodynamic total pressure is $(c_s^2+v_a^2/2)\rho$, and its vertical derivative is $-g\rho$. The magnetic pressure therefore increases the scale height above that of an unmagnetized atmosphere.

A magnetic buoyancy instability is a gravitational instability of a magnetized stratified fluid in which displacements of the gas and magnetic field can release Newtonian gravitational potential energy. Magnetic pressure supports part of the weight. Both interchange displacements and undular displacements can enter this broad category; Parker instability is the undular mechanism involving drainage along bent magnetic field lines.

Magnetoconvection is thermal convection coupled to the evolution and forces of a magnetic field. Conserved magnetic flux can supply a slow field that must be retained along with the convective complex amplitude, rather than being eliminated into a single local amplitude equation.

In the nonrelativistic scalar-conductivity approximation, neglecting Hall and other nonideal electromotive effects, $\mathbf{J}=\sigma (\mathbf{E}+\mathbf{u}\times \mathbf{B})$. The ideal finite-current limit gives $\mathbf{E}=-\mathbf{u}\times \mathbf{B}$ and hence the ideal magnetohydrodynamic induction equation.

The magnetic Reynolds number compares field advection with resistive magnetic diffusion. With constant electrical conductivity and vacuum permeability, magnetic diffusivity is ${\eta }_m=1/({\mu }_0\sigma )$ and $\mathrm{Rm}=UL/{\eta }_m$. The ideal induction approximation applies when this ratio is large on the scales of interest.

Finite electrical conductivity permits resistive smoothing of a magnetic field. With uniform coefficients and no motion the field satisfies a diffusion equation; with motion the diffusion term supplements the curl of $\mathbf{u}\times \mathbf{B}$. The magnetic Reynolds number compares these effects.

Resistive magnetohydrodynamics retains finite magnetic diffusivity in the coupled evolution of a conducting fluid and its magnetic field. The resistive induction equation allows field diffusion relative to the fluid, while the magnetohydrodynamic momentum equation includes the Lorentz force density. It contrasts with the zero-diffusivity limit of ideal magnetohydrodynamics.

For constant mass density $\rho$, kinematic viscosity $\nu$ and magnetic permeability ${\mu }_0$, the incompressible momentum equation isIt is the Navier-Stokes equation with Lorentz force density. The magnetic force decomposes into magnetic tension and a magnetic pressure gradient. A uniform streamwise pressure gradient need not make ordinary pressure independent of transverse coordinates.

For an isolated razor-thin disk, rescale its exterior magnetic scalar potential to satisfy $\sqrt{4\pi G/{\mu }_0}\mathbf{B}=-\nabla {\Phi }_M$. Comparing the normal magnetic boundary derivative with ${\partial }_z\Phi =2\pi G\Sigma$ identifies the displayed equivalent signed surface density. Both exterior potentials satisfy Laplace's equation. The equivalent surface density is a representation of the magnetic boundary data, rather than physical negative mass.

A lava lake is a persistent exposed body of molten or partly molten magma. Surface radiative cooling, thermal convection, latent heat, and internal radiogenic heating can jointly control formation and melting of its crust.

A circular, opaque, geometrically thin disk has projected area $\pi R^2|\cos i|$. For isotropically oriented normals, $|\cos i|$ is uniform on $[0,1]$, so the mean interception area is half the face-on area. A nonunit covering fraction multiplies this cross-section. Finite thickness, orientation-dependent absorption thresholds and incomplete coverage can change it; this is an average over randomly placed disks, not the inclination distribution conditional on an observed interception.

For a population with comoving number density $n_c$ and proper interception area ${\sigma }_p$, the absorption incidence is the proper density multiplied by cross-section and proper light-path length $cdz/[H(z)(1+z)]$. The displayed relation assumes one counted absorption system per interception. Completeness, covering fraction, evolution and the distinction between observed and rest-frame wavelength separation must be stated in an inference from a spectrum.

Orbital stability asks that a disturbance remain close to an invariant orbit or symmetry family, rather than to one fixed representative. In a complex Landau amplitude equation with $\beta =0$, $\mu >0$, $\lambda >0$, the circle $|A|=\sqrt{\mu /\lambda }$ attracts radial disturbances while every phase on it remains stationary. The family is attracting as a set, but its individual points do not have individual asymptotic stability because their phase is neutral.

A journal bearing supports a rotating axle inside a surrounding cylindrical sleeve with a thin lubricating film. An eccentric gap generates lubrication pressure as rotation transports fluid into and out of narrower regions. A full-film journal bearing model imposes periodic pressure around the entire circumference; a model with cavitation needs additional free-boundary conditions. The two models can predict different loads and dynamics.

A blade moving over a thin gravity-driven viscous film produces a moving-frame flux $\mathbf{q}=-h{\mathbf{e}}_x-h^3\nabla h/3$. Scaling film thickness by $h_0$ and horizontal distance by $\rho g{h}_0^3/(\mu U)$ yields this dimensionless volume-conservation equation. Fluid can escape beneath the blade or around its ends.