Character codex

  • Alfvena

    Equation
    \[v_A = \frac{B}{\sqrt{\mu_0 \rho}}\]

  • Arago

    Equation
    \[N_F = \frac{a^{2}}{\lambda L}\]

  • Areax

    Equation
    \[A_{\text{final}} \ge A_1 + A_2\]

  • Arnold's Cat

    Power
    Each step stretches the picture in one direction and squeezes it in another, keeping its area, so the cat quickly turns to noise.
    Equation
    \[\Gamma:\ (x, y) \mapsto (x + y,\ x + 2y) \bmod 1\]
    Year
    1968
    Scientist
    Vladimir Arnold
    Domain
    Waves, Chaos & Matter

  • Aurea

    Equation
    \[|\mathbf{k}\cdot\boldsymbol{\omega}| \ge \frac{\gamma}{|\mathbf{k}|^{\tau}}\]

  • Axona

    Equation
    \[C_m \frac{dV}{dt} = -\bar g_{Na} m^{3}h\,(V - E_{Na}) - \bar g_{K} n^{4}(V - E_K) - g_L (V - E_L) + I\]

  • Azurwake

    Power
    A charged particle moving through a medium faster than light travels in that medium emits light in a cone, like a sonic boom.
    Equation
    \[\cos\theta = \frac{1}{n\beta}, \qquad \beta > \frac{1}{n}\]
    Year
    1937
    Domain
    Forces & Fields

  • Bertrande

    Equation
    \[F = -\frac{k}{r^{2}} \quad \text{or} \quad F = -k\,r\]

  • Bifurcor

    Power
    A magnetic field that changes with height pushes on an atom's magnetic moment.
    Equation
    \[F_z = \mu_z\,\frac{\partial B_z}{\partial z}\]
    Year
    1922
    Domain
    Quantum

  • Bose-Einstein Condensate 1995 Tee

    Power
    Cool atoms until their quantum waves are as wide as the spaces between them, and thousands of them fall into the same lowest-energy state and act as one.
    Equation
    \[\lambda_{\mathrm{dB}} = \frac{h}{\sqrt{2\pi m k_B T}}\]
    Year
    1995
    Scientist
    Eric Cornell, Carl Wieman, Wolfgang Ketterle
    Domain
    Quantum

  • Bounda

    Equation
    \[S \le \frac{2\pi k_B R E}{\hbar c}\]

  • Bremsella

    Power
    Any accelerating charge radiates.
    Equation
    \[P = \frac{q^2 a^2}{6\pi\varepsilon_0 c^3}\]
    Year
    1897
    Domain
    Forces & Fields

  • Casimira

    Power
    Quantum vacuum fluctuations between two close, parallel, uncharged metal plates are restricted, so the plates are pulled together.
    Equation
    \[\frac{F}{A} = -\frac{\pi^2\hbar c}{240\,d^4}\]
    Year
    1948
    Domain
    Quantum

  • Cavenda

    Equation
    \[F = \frac{G M m}{r^{2}}, \qquad \kappa\theta = F L, \qquad T = 2\pi\sqrt{\frac{I}{\kappa}}\]

  • Celtrix

    Equation
    \[\frac{d\mathbf{L}}{dt} = \mathbf{r}_c \times \mathbf{F}_c\]

  • Chandrasekhar Limit Tee: 1.4 M☉

    Power
    In a white dwarf, electrons refuse to share quantum states and push back, holding the star up.
    Equation
    \[M_{\mathrm{Ch}} = \frac{\omega_3^{0}\sqrt{3\pi}}{2}\left(\frac{\hbar c}{G}\right)^{3/2}\frac{1}{(\mu_e m_H)^{2}} \approx \frac{5.8\,M_\odot}{\mu_e^{2}}\]
    Year
    1931
    Scientist
    Subrahmanyan Chandrasekhar
    Domain
    Relativity & Cosmos

  • Choralis

    Equation
    \[\Gamma(\theta) = \frac{1}{2} - \frac{x}{4} + \frac{3}{2}\,x\ln x, \qquad x = \frac{1-\cos\theta}{2}\]

  • Chuanna

    Equation
    \[\frac{dx}{dt} = \alpha\,(y - x - f(x)), \qquad \frac{dy}{dt} = x - y + z, \qquad \frac{dz}{dt} = -\beta y\]

  • Condensa

    Power
    Below a critical temperature, a gas of bosons starts collecting in its lowest quantum state.
    Equation
    \[\frac{N_0}{N} = 1 - \left(\frac{T}{T_c}\right)^{3/2}\quad(T\le T_c)\]
    Year
    1925
    Domain
    Quantum

  • Corekeeper

    Power
    Yukawa proposed that nucleons attract by exchanging a massive particle.
    Equation
    \[V(r) = -\frac{g^{2}}{4\pi}\frac{e^{-r/\lambda}}{r}, \qquad \lambda = \frac{\hbar}{m_\pi c}\]
    Year
    1935
    Scientist
    Murray Gell-Mann, Richard Feynman
    Domain
    Forces & Fields

  • Coriolix

    Power
    In a rotating frame, moving objects appear to be pushed sideways by the Coriolis term, −2Ω × v.
    Equation
    \[\mathbf{a}' = -2\,\boldsymbol{\Omega}\times\mathbf{v}' - \boldsymbol{\Omega}\times(\boldsymbol{\Omega}\times\mathbf{r}')\]
    Year
    1835
    Domain
    Waves, Chaos & Matter

  • Cryo Fault

    Power
    Griffith showed that a crack grows when the elastic energy it releases is enough to pay for the new surface it creates.
    Equation
    \[\sigma_f = \sqrt{\frac{2E\gamma_s}{\pi a}}\]
    Year
    1921
    Scientist
    Alan Arnold Griffith
    Domain
    Waves, Chaos & Matter, Heat & Entropy

  • Dark Matter Host

    Power
    When two galaxy clusters collided in the Bullet Cluster, their hot gas slammed together and stalled, but bent background light shows most of the mass sailed on with the galaxies.
    Equation
    \[v(r)^{2} = \frac{G M(r)}{r} \;\Rightarrow\; M(r) = \frac{v^{2} r}{G}\]
    Year
    1937
    Scientist
    Albert Einstein, Isaac Newton, Vera Rubin
    Domain
    Relativity & Cosmos

  • Decay Dancer

    Power
    A free neutron decays into a proton, an electron and an antineutrino, because one down quark turns into an up quark by emitting a W boson.
    Equation
    \[n \to p + e^{-} + \bar\nu_e\]
    Year
    1934
    Scientist
    Enrico Fermi
    Domain
    Forces & Fields

  • Decoherex

    Power
    The off-diagonal terms in a density matrix carry the ability to interfere.
    Equation
    \[\rho_{01}(t) = \rho_{01}(0)\,e^{-t/\tau_D}\]
    Year
    1970
    Scientist
    Wojciech Zurek
    Domain
    Quantum

  • Diagonix

    Power
    A polarizer passes the fraction cos²θ of already-polarized light.
    Equation
    \[I = I_0\cos^2\theta\]
    Year
    1809
    Domain
    Forces & Fields

  • Ehrenwheel

    Equation
    \[C' = \frac{2\pi R}{\sqrt{1-\omega^{2}R^{2}/c^{2}}} > 2\pi R\]

  • Ekmara

    Equation
    \[u + iv = V_0\,e^{i\pi/4}\,e^{(1+i)z/D}, \qquad z \le 0\]

  • Erasa

    Equation
    \[\langle Q \rangle \ge k_B T \ln 2\]

  • Eventide Prophet

    Power
    Hawking showed that black holes glow faintly, with a temperature that goes down as their mass goes up.
    Equation
    \[T_H = \frac{\hbar c^{3}}{8\pi G M k_B}\]
    Year
    1975
    Scientist
    Jacob Bekenstein, Stephen Hawking
    Domain
    Relativity & Cosmos

  • Exclusor

    Power
    Electrons are fermions, so their joint wavefunction must change sign when two are swapped.
    Equation
    \[\psi(x_1,x_2) = \frac{1}{\sqrt{2}}\begin{vmatrix} \phi_a(x_1) & \phi_b(x_1) \\ \phi_a(x_2) & \phi_b(x_2) \end{vmatrix}\]
    Year
    1925
    Scientist
    Wolfgang Pauli
    Domain
    Quantum

  • Expulsieur

    Power
    A superconductor expels magnetic field from its interior, which a merely perfect conductor would not do.
    Equation
    \[\mathbf{B}_{\text{inside}} = 0\]
    Year
    1935
    Domain
    Quantum

  • Fermia

    Equation
    \[N = R_{*}\cdot f_p \cdot n_e \cdot f_l \cdot f_i \cdot f_c \cdot L\]

  • Flagella

    Equation
    \[F = A v + B\Omega, \qquad N = B v + D\Omega\]

  • Foldara

    Equation
    \[3^{100} \approx 5\times10^{47} \ \text{shapes}\]

  • Gamowyn

    Equation
    \[\text{rate} \propto e^{-E/kT}\, e^{-\sqrt{E_G/E}}\]

  • Glueba

    Equation
    \[\text{Prove: quantum Yang–Mills theory exists on } \mathbb{R}^{4} \text{ with mass gap } \Delta > 0\]

  • Graviton Whisper

    Power
    Far from strong sources, Einstein's equations reduce to a wave equation: moving masses send out ripples in spacetime that travel at the speed of light.
    Equation
    \[\Box\,\bar h_{\mu\nu} = -\frac{16\pi G}{c^{4}}\,T_{\mu\nu}\]
    Year
    1916
    Scientist
    Matvei Bronstein, Richard Feynman
    Domain
    Relativity & Cosmos

  • Gyrolla

    Power
    A magnetic field bends a charged particle into a circle without changing its speed.
    Equation
    \[q v B = \frac{m v^2}{r} \;\Rightarrow\; r = \frac{m v}{q B}\]
    Year
    1932
    Domain
    Forces & Fields

  • Hadron Brawler

    Power
    The Cornell potential describes the force between a heavy quark and antiquark: Coulomb-like at short range, with an extra term that grows steadily with distance.
    Equation
    \[V(r) = -\frac{4}{3}\frac{\alpha_s \hbar c}{r} + \sigma r\]
    Year
    1975
    Scientist
    Murray Gell-Mann
    Domain
    Forces & Fields

  • Helia

    Equation
    \[H = \tfrac{1}{2}\left(p_x^{2} + p_y^{2}\right) + \tfrac{1}{2}\left(x^{2} + y^{2}\right) + x^{2}y - \tfrac{1}{3}y^{3}\]

  • Homopole

    Equation
    \[\mathcal{E} = \int (\mathbf{v}\times\mathbf{B})\cdot d\mathbf{r} = \tfrac{1}{2} B\,\omega R^{2}\]

  • Ignia

    Equation
    \[n\,T\,\tau_E \gtrsim 3\times10^{21}\ \mathrm{keV\,s\,m^{-3}} \quad (\text{D-T ignition; lowest near } T \approx 14\ \mathrm{keV})\]

  • Interfera

    Power
    When a particle can reach the screen by two paths, you add the amplitudes before squaring them, and the cross term creates bright and dark fringes.
    Equation
    \[P = \lvert\psi_1 + \psi_2\rvert^{2} = \lvert\psi_1\rvert^{2} + \lvert\psi_2\rvert^{2} + 2\,\mathrm{Re}\!\left(\psi_1^{*}\psi_2\right)\]
    Year
    1976
    Scientist
    Richard Feynman, Thomas Young
    Domain
    Quantum

  • Invertia

    Power
    Temperature is defined by how entropy changes when you add energy.
    Equation
    \[\frac{1}{T} = \frac{\partial S}{\partial E} < 0\]
    Year
    1951
    Domain
    Heat & Entropy

  • Jarza

    Equation
    \[\langle e^{-\beta W}\rangle = e^{-\beta\Delta F}, \qquad \beta = \frac{1}{k_B T}\]

  • Jetlagga

    Equation
    \[\text{Eastward: observed } -59 \pm 10\ \mathrm{ns}, \quad \text{predicted } -40 \pm 23\ \mathrm{ns}\]

  • Kayella

    Equation
    \[\eta = K\,\dot{\gamma}^{\,n-1}, \qquad n < 1 \ (\text{shear-thinning})\]

  • Kelvinor

    Equation
    \[t = \frac{T_0^{2}}{\pi\,\kappa\,G^{2}} \qquad (\text{cooling by conduction only})\]

  • Kilonova

    Equation
    \[\Delta t = 1.74 \pm 0.05\ \mathrm{s}\]

  • Kinessa

    Equation
    \[W = F \times d = 6\ \mathrm{pN} \times 8\ \mathrm{nm} = 48\ \mathrm{pN\,nm}\]

  • Kochenspek

    Equation
    \[\text{18 vectors, 9 orthogonal bases, each vector in 2 bases (4 dimensions)}\]

  • Lenta

    Equation
    \[v_g = \frac{c}{n + \omega\,\dfrac{dn}{d\omega}}\]

  • Lenzor

    Power
    A changing magnetic flux induces a voltage, and the induced current always flows so as to oppose the change.
    Equation
    \[\mathcal{E} = -\frac{d\Phi_B}{dt}\]
    Year
    1834
    Domain
    Forces & Fields

  • Levitah

    Equation
    \[U = \frac{4\pi}{3}a^{3}\left[f_1\,\tfrac{1}{2}\kappa_0\langle p^{2}\rangle - f_2\,\tfrac{3}{4}\rho_0\langle v^{2}\rangle\right]\]

  • Libratrix

    Power
    Two bodies orbiting each other have five points where a small third body can keep pace with them.
    Equation
    \[r_{L2} \approx R\left(\frac{M_2}{3M_1}\right)^{1/3}\]
    Year
    1772
    Domain
    Waves, Chaos & Matter, Forces & Fields

  • Lumidisk

    Equation
    \[\oint \mathbf{E}\cdot d\mathbf{l} = -\frac{d\Phi_B}{dt}\]

  • Magnara

    Power
    A spinning ball moving through air is pushed sideways, toward the side where its surface moves with the airflow.
    Equation
    \[\mathbf{F}_M = \alpha\,\boldsymbol{\omega}\times\mathbf{v}\]
    Year
    1853
    Domain
    Waves, Chaos & Matter

  • Magnetron Twins

    Power
    The energy of two small magnets depends on both their distance and how they are oriented relative to the line joining them.
    Equation
    \[U = -\frac{\mu_0}{4\pi r^{3}}\left[3(\vec m_1\cdot\hat r)(\vec m_2\cdot\hat r) - \vec m_1\cdot\vec m_2\right]\]
    Year
    1873
    Scientist
    James Clerk Maxwell
    Domain
    Forces & Fields

  • Marina Dirac

    Equation
    \[\left(i\hbar\,\gamma^{\mu}\partial_{\mu} - mc\right)\psi = 0\]

  • Moderon

    Power
    A neutron loses the largest share of its energy when it hits a nucleus of about its own mass.
    Equation
    \[\alpha = \left(\frac{A-1}{A+1}\right)^2\]
    Year
    1935
    Domain
    Forces & Fields

  • Molassa

    Equation
    \[k_B T_D = \frac{\hbar\Gamma}{2} \qquad (\text{two-level atom, best at } \delta = -\Gamma/2)\]

  • Monopola

    Equation
    \[e\,g = \frac{n\hbar c}{2} \qquad (\text{Gaussian units},\ n = 0, \pm1, \pm2, \dots)\]

  • Mossbra

    Equation
    \[E_R = \frac{E_\gamma^{2}}{2Mc^{2}}\]

  • Muonaut

    Power
    Muons made high in the atmosphere live only about two microseconds, too short to cross the atmosphere at face value.
    Equation
    \[\Delta t = \gamma\,\tau, \qquad L = \frac{L_0}{\gamma}\]
    Year
    1941
    Domain
    Relativity & Cosmos

  • Murmura

    Equation
    \[2\pi R \approx m\lambda \qquad (m \text{ large})\]

  • Navia

    Equation
    \[\rho\left(\frac{\partial \mathbf{u}}{\partial t} + (\mathbf{u}\cdot\nabla)\mathbf{u}\right) = -\nabla p + \mu\nabla^{2}\mathbf{u}\]

  • Neutrina Fade

    Power
    A charged particle moving through water faster than light moves in water gives off a cone of blue Cherenkov light, at an angle set by its speed and the refractive index.
    Equation
    \[\cos\theta_C = \frac{1}{n\beta}\]
    Year
    1937
    Scientist
    Enrico Fermi, Wolfgang Pauli
    Domain
    Forces & Fields

  • Nickela

    Equation
    \[d\sin\phi = \lambda, \quad d = 0.215\ \mathrm{nm} \ \Rightarrow\ \lambda = 0.165\ \mathrm{nm}\]

  • Nocturna

    Equation
    \[dN_{\star} \propto r^{2}\,dr, \qquad F_{\star} \propto \frac{1}{r^{2}} \ \Rightarrow\ dF_{\text{shell}} \propto dr\]

  • Null Beacon

    Power
    In a universe whose expansion is speeding up, there is a largest distance from which light sent today can ever reach us: about 16.7 billion light-years.
    Equation
    \[d_{\text{EH}}(t) = a(t)\int_{t}^{\infty} \frac{c\,dt^{\prime}}{a(t^{\prime})}\]
    Year
    1956
    Domain
    Relativity & Cosmos