Character codex

  • Alfvena

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

  • Arago

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

  • Areax

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

  • Arnold's Cat

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

  • Aurea

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

  • Axona

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

  • Azurwake

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

  • Bertrande

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

  • Bifurcor

    Kraft
    A magnetic field that changes with height pushes on an atom's magnetic moment.
    Ekvation
    \[F_z = \mu_z\,\frac{\partial B_z}{\partial z}\]
    År
    1922
    Område
    Quantum

  • Bose-Einstein Condensate 1995 Tee

    Kraft
    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.
    Ekvation
    \[\lambda_{\mathrm{dB}} = \frac{h}{\sqrt{2\pi m k_B T}}\]
    År
    1995
    Forskare
    Eric Cornell, Carl Wieman, Wolfgang Ketterle
    Område
    Quantum

  • Bounda

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

  • Bremsella

    Kraft
    Any accelerating charge radiates.
    Ekvation
    \[P = \frac{q^2 a^2}{6\pi\varepsilon_0 c^3}\]
    År
    1897
    Område
    Forces & Fields

  • Casimira

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

  • Cavenda

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

  • Celtrix

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

  • Chandrasekhar Limit Tee: 1.4 M☉

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

  • Choralis

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

  • Chuanna

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

  • Condensa

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

  • Corekeeper

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

  • Coriolix

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

  • Cryo Fault

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

  • Dark Matter Host

    Kraft
    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.
    Ekvation
    \[v(r)^{2} = \frac{G M(r)}{r} \;\Rightarrow\; M(r) = \frac{v^{2} r}{G}\]
    År
    1937
    Forskare
    Albert Einstein, Isaac Newton, Vera Rubin
    Område
    Relativity & Cosmos

  • Decay Dancer

    Kraft
    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.
    Ekvation
    \[n \to p + e^{-} + \bar\nu_e\]
    År
    1934
    Forskare
    Enrico Fermi
    Område
    Forces & Fields

  • Decoherex

    Kraft
    The off-diagonal terms in a density matrix carry the ability to interfere.
    Ekvation
    \[\rho_{01}(t) = \rho_{01}(0)\,e^{-t/\tau_D}\]
    År
    1970
    Forskare
    Wojciech Zurek
    Område
    Quantum

  • Diagonix

    Kraft
    A polarizer passes the fraction cos²θ of already-polarized light.
    Ekvation
    \[I = I_0\cos^2\theta\]
    År
    1809
    Område
    Forces & Fields

  • Ehrenwheel

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

  • Ekmara

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

  • Erasa

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

  • Eventide Prophet

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

  • Exclusor

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

  • Expulsieur

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

  • Fermia

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

  • Flagella

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

  • Foldara

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

  • Gamowyn

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

  • Glueba

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

  • Graviton Whisper

    Kraft
    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.
    Ekvation
    \[\Box\,\bar h_{\mu\nu} = -\frac{16\pi G}{c^{4}}\,T_{\mu\nu}\]
    År
    1916
    Forskare
    Matvei Bronstein, Richard Feynman
    Område
    Relativity & Cosmos

  • Gyrolla

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

  • Hadron Brawler

    Kraft
    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.
    Ekvation
    \[V(r) = -\frac{4}{3}\frac{\alpha_s \hbar c}{r} + \sigma r\]
    År
    1975
    Forskare
    Murray Gell-Mann
    Område
    Forces & Fields

  • Helia

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

  • Homopole

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

  • Ignia

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

  • Interfera

    Kraft
    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.
    Ekvation
    \[P = \lvert\psi_1 + \psi_2\rvert^{2} = \lvert\psi_1\rvert^{2} + \lvert\psi_2\rvert^{2} + 2\,\mathrm{Re}\!\left(\psi_1^{*}\psi_2\right)\]
    År
    1976
    Forskare
    Richard Feynman, Thomas Young
    Område
    Quantum

  • Invertia

    Kraft
    Temperature is defined by how entropy changes when you add energy.
    Ekvation
    \[\frac{1}{T} = \frac{\partial S}{\partial E} < 0\]
    År
    1951
    Område
    Heat & Entropy

  • Jarza

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

  • Jetlagga

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

  • Kayella

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

  • Kelvinor

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

  • Kilonova

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

  • Kinessa

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

  • Kochenspek

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

  • Lenta

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

  • Lenzor

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

  • Levitah

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

  • Libratrix

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

  • Lumidisk

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

  • Magnara

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

  • Magnetron Twins

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

  • Marina Dirac

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

  • Moderon

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

  • Molassa

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

  • Monopola

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

  • Mossbra

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

  • Muonaut

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

  • Murmura

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

  • Navia

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

  • Neutrina Fade

    Kraft
    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.
    Ekvation
    \[\cos\theta_C = \frac{1}{n\beta}\]
    År
    1937
    Forskare
    Enrico Fermi, Wolfgang Pauli
    Område
    Forces & Fields

  • Nickela

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

  • Nocturna

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

  • Null Beacon

    Kraft
    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.
    Ekvation
    \[d_{\text{EH}}(t) = a(t)\int_{t}^{\infty} \frac{c\,dt^{\prime}}{a(t^{\prime})}\]
    År
    1956
    Område
    Relativity & Cosmos