In Anti-Stokes Raman scattering, matter loses internal energy and the outgoing photon gains it. The harmonic transition $v\to v-1$ requires $v\ge 1$, so an initially excited vibrational population must be available. At low temperature, high-frequency vibrational excitations are scarce and the corresponding anti-Stokes line is weak. The extra photon energy comes from the molecule; there is no conflict with conservation of energy.

In Stokes Raman scattering, matter gains internal energy and the photon loses the same amount. For a quantum harmonic oscillator representing one molecular vibration, $E_v=h{\nu }_v(v+1/2)$ with $v=0,1,\dots$. The transition $v\to v+1$ gives ${\nu }_s={\nu }_0-{\nu }_v$, requiring ${\nu }_0>{\nu }_v$ for an outgoing photon. Even a molecule initially in its vibrational ground state can undergo this process. The shared name does not turn it into the absorption/emission-band Stokes shift used for fluorescence.

The signed Raman shift subtracts scattered from incident spectroscopic wavenumber:Here $c$ is the speed of light, and both wavelengths are in vacuum. Positive shifts denote Stokes Raman scattering; negative shifts denote Anti-Stokes Raman scattering. Some plots reverse the horizontal direction or report separate unsigned magnitudes, so check the convention. Spectroscopic wavenumber has no $2\pi$ factor, unlike the common angular wavenumber $k=2\pi /\lambda$. A shift of $1000\mathrm{c}{\mathrm{m}}^{-1}$ means $100000{\mathrm{m}}^{-1}$, not a frequency of $1000\mathrm{Hz}$.

For a one-quantum change of molecular vibration with ordinary frequency ${\nu }_v$, the magnitude is ${\tilde{\nu }}_v={\nu }_v/c$. This makes Raman spectroscopy attractive: the same molecular energy spacing can be read using different visible excitation wavelengths. Equal and opposite Raman shifts are not equal and opposite changes measured in nanometres, because wavelength is the reciprocal of spectroscopic wavenumber.

Chandrasekhara Venkata Raman and Kariamanikkam Srinivasa Krishnan jointly reported the effect in 1928. Their letter describes light from the Sun concentrated by an $18\mathrm{cm}$-aperture, $230\mathrm{cm}$-focal length telescope objective and a second optical lens onto a liquid purified by repeated vacuum distillation. With blue-violet and yellow-green optical filters together in the incident beam, the visible track disappeared; moving the yellow-green optical filter between liquid and observer restored it. The complementary arrangement rejected unchanged-colour scattering of light while admitting newly generated light. Persistence after purification and strong wave polarization in many liquids argued against ordinary fluorescent contamination.^[ref]

In his 1930 lecture, Chandrasekhara Venkata Raman describes a cobalt-glass optical filter selecting indigo-violet light from the Sun, with a separated blue-green band in the scattered optical spectrum. Substituting a quartz mercury arc and condenser gave sharp new spectral lines. Small Hilger quartz spectrographs recorded them photographically; Kariamanikkam Srinivasa Krishnan obtained more precise records with a larger instrument and established violet-displaced lines. The optical prism disperses wavelengths for spatial readout; it does not create the Raman shift. The diagram gives functional optical paths rather than a reconstruction of a specific Hilger instrument.^[ref]

Their May 1928 report strengthens the comparison: filtered mercury illumination of toluene produced extra spectral lines. Removing the $4358\text{A˚}$ incident line removed its associated longer-wavelength group; a quinine filter removing the $4047$, $4078$ and $4109\text{A˚}$ group removed a different shifted group while preserving the one associated with $4358\text{A˚}$. These are actual selective-excitation controls, rather than inferred colours.^[ref]

The inference has limits. A complementary-filter test alone establishes newly admitted wavelengths, not their precise spacing or a unique microscopic mechanism. Fluorescence can also survive purification when intrinsic to the liquid, and fluorescence can be polarized. Useful distinctions therefore combine resolved spectral lines, excitation dependence, wave polarization and sample preparation. A proposed modern extension is to change a single incident frequency: a molecular Raman shift should follow the same internal energy gap, whereas ordinary relaxed molecular fluorescence usually retains approximately its emission-band positions. This is a diagnostic under stated conditions, not a universal theorem about every fluorescent material or resonant scattering process. Raman scattering need not involve a populated, relaxed electronic excited state as ordinary molecular fluorescence does; neither a redder photon nor the word Stokes identifies the mechanism by itself.

The 1930 Nobel Prize in Physics went to Chandrasekhara Venkata Raman alone for his work on scattering of light and the discovery of the effect. That award allocation should be distinguished from the joint experimental report with Kariamanikkam Srinivasa Krishnan.^[ref]

For a stable radiometer with affine output $S=g(T+T_r)$, let $g>0$ be the fixed response coefficient and $T_r$ the receiver noise temperature. Two reference loads with known equivalent input noise temperatures $T_c<T_h$ give outputs $S_c$ and $S_h$. Subtracting their outputs eliminates $T_r$; dividing source and reference differences eliminates $g$:This two-load radiometer calibration assumes unchanged response and receiver noise temperature between readings, with the loads and source referred to the same input. It also eliminates an additional constant output offset. Physical load temperatures must first be converted to the applicable equivalent input noise temperatures when the classical thermal approximation fails. The Penzias-Wilson microwave background experiment gives an original worked example.

A noise temperature expresses received or internally added noise power on an equivalent temperature scale. For one matched receiving channel in the classical thermal limit, an ideal rectangular bandwidth $\Delta \nu$ gives $P=k_{\mathrm{B}}{T}_N\Delta \nu$, with Boltzmann constant $k_{\mathrm{B}}$. An equivalent noise temperature need not equal a component's physical temperature.

Radiocarbon calibration converts conventional radiocarbon ages into calendar-age information using independently dated material and models of changes in reservoir isotope ratios. Conventional ages use the historical $5568$-year half-life, whereas the physical carbon-14 half-life is about $5730$ years.^[ref]

A radiocarbon age estimates elapsed time from a measured carbon-14 ratio $R$, an assumed initial ratio $R_0$ and a specified nuclear decay constant $\lambda$. The displayed exponential decay inversion gives the age on that model's timescale. A conventional radiocarbon age uses a prescribed reference and decay convention; it is not generally a calendar age. Radiocarbon calibration accounts for changes in the atmospheric isotope ratio and maps the measurement to a calendar-age estimate.

Aperture synthesis reconstructs the sky's brightness from complex visibilities measured at different interferometric baselines. Each measurement constrains a Fourier transform component of the brightness, rather than supplying a little photograph. Combining many such components can distinguish sources that each individual antenna leaves unresolved. The remarkable economy is that changing separations and the rotation of Earth can provide many measurements with only a few physical antennas.

Martin Ryle's Cambridge group made aperture synthesis a practical method of astronomical imaging at the Mullard Radio Astronomy Observatory. Cambridge's institutional history connects that work with the One-Mile Telescope and its larger successors.^[ref]

In his 1974 lecture Radio Telescopes of Large Resolving Power, Martin Ryle recalled the problem of distinguishing weak extragalactic sources and resolving their structure. He explained sequential wavefront sampling using one simultaneously observed element as a wave phase reference, and the saving obtained by letting Earth rotate the apparent baseline.^[ref]

The 1974 Nobel Prize in Physics distinguished Martin Ryle's observations and inventions, especially aperture synthesis, from Antony Hewish's role in discovering pulsars. The latter is a separate astronomical discovery, with its own observational history.^[ref]

Interplanetary scintillation is rapid variation in the received strength of a compact astronomical radio source, produced by propagation through fluctuating electron density in the solar wind. Its dependence on source angular size can help distinguish compact sources. It is a propagation effect, distinct from intrinsic periodic emission by a pulsar.

A radio telescope is an astronomical instrument that receives radio waves using an antenna and associated receivers. A single dish measures radiation over its directional sensitivity pattern; separated elements can supply complex visibilities for aperture synthesis.

For $\ddot{x}+x-\epsilon \stackrel{...}{x}=f$ and the $e^{-i\omega t}$ convention, the frequency response is $G(\omega )=[1-{\omega }^2-i\epsilon {\omega }^3{]}^{-1}$. At small nonzero real $\epsilon$, its poles areFor positive $\epsilon$ the slow oscillations decay but the fast mode runs away; for negative $\epsilon$ the fast mode decays but the slow oscillations grow. Thus no nonzero sign makes all modes stable. A causal initial-value response and a bounded response free of runaways impose different boundary conditions.

For positive $\epsilon$, the real-axis frequency response of the radiation-reaction oscillator pole structure excludes future runaway growth but retains an upper-half-plane pole. Closing its inverse Fourier transform upward at $t<0$ gives a nonzero response before the force. The fast pole contributes approximately $\epsilon e^{t/\epsilon }$ for negative $t$. A strictly causal retarded prescription instead includes an exponentially growing term for positive $t$ and requires a Laplace transform contour. The pre-response is a consequence of imposing boundedness at future infinity, not an unavoidable property of all initial-value solutions of the differential equation.

For $|\epsilon \omega |\ll 1$, use the zeroth-order equation $\ddot{x}=f-x$ inside the small third-derivative term, givingFor positive $\epsilon$ this reduced equation has a stable retarded response with no high-frequency runaway. Its response $G_{\mathrm{red}}=(1-i\epsilon \omega )/(1-{\omega }^2-i\epsilon \omega )$ agrees with the unreduced oscillator to first order at fixed nonresonant frequency. Order reduction deliberately removes the singular fast mode outside the assumed low-frequency regime; it is an approximation rather than an exact alternative boundary condition for the third-order equation.

An ideal point emitter emits radiant flux from one location. It approximates a physical source when its emitting dimensions are small relative to the distances relevant to the calculation. With isotropy, its radiant intensity is $I=\Phi /(4\pi )$ for total radiant flux $\Phi$. An extended source generally requires integrating contributions from different emitting positions.

For positive $Z$, the displayed identity follows by differentiating $Z^n=e^{n\log Z}$ at zero.

Integer powers of a partition function represent independent copies with the same disorder. Integer moments alone do not justify analytic continuation or interchanging disorder averages and thermodynamic limits.^[ref]

Choose two Ising spins with Hamiltonian $H=-J{s}_1{s}_2$, where $J$ independently takes $J_0$ or $2J_0$ with equal prior probabilities and $J_0>0$. This original finite example has no geometrical frustration and no phase transition. Its four spin assignments give $Z_J=4\cosh (\beta J)$. ThereforeThe concave function $\log$ puts $F_{\mathrm{a}}\le F_{\mathrm{q}}$. For this two-value case the claim is just $(Z_1+Z_2)/2\ge \sqrt{Z_1{Z}_2}$, obtained by squaring $\sqrt{Z_1}-\sqrt{Z_2}$. Thus no formal continuation of replicas is needed to see the distinction.

In the annealed disorder ensemble, the stronger bond has probability $Z_{2J_0}/(Z_{J_0}+Z_{2J_0})$, approaching one at low temperature. A quenched disorder collection instead retains one half at each coupling. As $T\to 0$, $F_{\mathrm{q}}\to -3J_0/2$ and $F_{\mathrm{a}}\to -2J_0$: averaging samples and allowing the material variables to equilibrate describe different physics.

Single-photon electron-positron annihilation can directly form quarkonium with $J^{PC}=1^{--}$. A vector S-wave quarkonium can annihilate back through a virtual photon into a charged-lepton pair. At leading nonrelativistic order, its electronic partial decay width is proportional to ${\alpha }^2{Q}_q^2|\psi (0){|}^2/M^2$, where the wavefunction at the origin describes the quark-antiquark annihilation overlap.

Below the threshold for a pair of heavy-light mesons, hadronic decays require annihilation, primarily into three gluons for a color-singlet $1^{--}$ state. One gluon cannot carry a color-singlet initial state, and two gluons have the wrong charge-conjugation parity. Above the heavy-light pair threshold, a strong interaction can instead separate the heavy quark and antiquark into different mesons after creating a light pair. This can greatly increase the total decay width without comparably changing the short-distance electronic partial width. A specific example is the contrast between the first three Upsilon mesons and the $4S$ state. Higher radial states can additionally undergo hadronic or radiative transitions to lower quarkonium states.

A particularly economical example is the baryon decuplet. Restrict to fully symmetric three-quark flavor states. The nonnegative occupation numbers satisfy $n_u+n_d+n_s=3$, giving $\left(\genfrac{}{}{0ex}{}{3+3-1}{3}\right)=10$ possibilities by stars and bars. Their additive labels areThese formulas follow directly from the constituent table. With fixed $n_s$, there are $4-n_s$ possible values of $n_u$, so the weight diagram has rows of four, three, two and one states. Its outer triangle is therefore a consequence of the constituent construction, rather than an arbitrary drawing convention.

The bottom corner has $n_s=3$, hence $I_3=0$, $Y=-2$ and $Q=-1$: the Omega baryon position. The top-right corner has $uuu$ and $Q=2$, corresponding to the doubly charged Delta baryon. Every point satisfies the Gell-Mann--Nishijima formula $Q=I_3+Y/2$.

The flavor construction is only part of the state. The Pauli constraint on three-quark flavour multiplets also involves spin angular momentum, the spatial wavefunction and color charge. In particular, three identical fermions cannot be assigned a completely symmetric total state merely because the flavor diagram is symmetric. Nor does the same flavor diagram determine the hadron masses: an approximate flavor symmetry can organize a spectrum without making all its members degenerate.

Quantum tunnelling between different energy bands, including transfer between the valence band and conduction band in a tunnel diode.