Character codex

  • Alfvena

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

  • Arago

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

  • Areax

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

  • Arnold's Cat

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

  • Aurea

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

  • Axona

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

  • Azurwake

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

  • Bertrande

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

  • Bifurcor

    Moc
    A magnetic field that changes with height pushes on an atom's magnetic moment.
    Równanie
    \[F_z = \mu_z\,\frac{\partial B_z}{\partial z}\]
    Rok
    1922
    Dziedzina
    Quantum

  • Bose-Einstein Condensate 1995 Tee

    Moc
    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.
    Równanie
    \[\lambda_{\mathrm{dB}} = \frac{h}{\sqrt{2\pi m k_B T}}\]
    Rok
    1995
    Naukowiec
    Eric Cornell, Carl Wieman, Wolfgang Ketterle
    Dziedzina
    Quantum

  • Bounda

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

  • Bremsella

    Moc
    Any accelerating charge radiates.
    Równanie
    \[P = \frac{q^2 a^2}{6\pi\varepsilon_0 c^3}\]
    Rok
    1897
    Dziedzina
    Forces & Fields

  • Casimira

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

  • Cavenda

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

  • Celtrix

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

  • Chandrasekhar Limit Tee: 1.4 M☉

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

  • Choralis

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

  • Chuanna

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

  • Condensa

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

  • Corekeeper

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

  • Coriolix

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

  • Cryo Fault

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

  • Dark Matter Host

    Moc
    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.
    Równanie
    \[v(r)^{2} = \frac{G M(r)}{r} \;\Rightarrow\; M(r) = \frac{v^{2} r}{G}\]
    Rok
    1937
    Naukowiec
    Albert Einstein, Isaac Newton, Vera Rubin
    Dziedzina
    Relativity & Cosmos

  • Decay Dancer

    Moc
    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.
    Równanie
    \[n \to p + e^{-} + \bar\nu_e\]
    Rok
    1934
    Naukowiec
    Enrico Fermi
    Dziedzina
    Forces & Fields

  • Decoherex

    Moc
    The off-diagonal terms in a density matrix carry the ability to interfere.
    Równanie
    \[\rho_{01}(t) = \rho_{01}(0)\,e^{-t/\tau_D}\]
    Rok
    1970
    Naukowiec
    Wojciech Zurek
    Dziedzina
    Quantum

  • Diagonix

    Moc
    A polarizer passes the fraction cos²θ of already-polarized light.
    Równanie
    \[I = I_0\cos^2\theta\]
    Rok
    1809
    Dziedzina
    Forces & Fields

  • Ehrenwheel

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

  • Ekmara

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

  • Erasa

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

  • Eventide Prophet

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

  • Exclusor

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

  • Expulsieur

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

  • Fermia

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

  • Flagella

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

  • Foldara

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

  • Gamowyn

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

  • Glueba

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

  • Graviton Whisper

    Moc
    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.
    Równanie
    \[\Box\,\bar h_{\mu\nu} = -\frac{16\pi G}{c^{4}}\,T_{\mu\nu}\]
    Rok
    1916
    Naukowiec
    Matvei Bronstein, Richard Feynman
    Dziedzina
    Relativity & Cosmos

  • Gyrolla

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

  • Hadron Brawler

    Moc
    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.
    Równanie
    \[V(r) = -\frac{4}{3}\frac{\alpha_s \hbar c}{r} + \sigma r\]
    Rok
    1975
    Naukowiec
    Murray Gell-Mann
    Dziedzina
    Forces & Fields

  • Helia

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

  • Homopole

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

  • Ignia

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

  • Interfera

    Moc
    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.
    Równanie
    \[P = \lvert\psi_1 + \psi_2\rvert^{2} = \lvert\psi_1\rvert^{2} + \lvert\psi_2\rvert^{2} + 2\,\mathrm{Re}\!\left(\psi_1^{*}\psi_2\right)\]
    Rok
    1976
    Naukowiec
    Richard Feynman, Thomas Young
    Dziedzina
    Quantum

  • Invertia

    Moc
    Temperature is defined by how entropy changes when you add energy.
    Równanie
    \[\frac{1}{T} = \frac{\partial S}{\partial E} < 0\]
    Rok
    1951
    Dziedzina
    Heat & Entropy

  • Jarza

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

  • Jetlagga

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

  • Kayella

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

  • Kelvinor

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

  • Kilonova

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

  • Kinessa

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

  • Kochenspek

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

  • Lenta

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

  • Lenzor

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

  • Levitah

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

  • Libratrix

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

  • Lumidisk

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

  • Magnara

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

  • Magnetron Twins

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

  • Marina Dirac

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

  • Moderon

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

  • Molassa

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

  • Monopola

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

  • Mossbra

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

  • Muonaut

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

  • Murmura

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

  • Navia

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

  • Neutrina Fade

    Moc
    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.
    Równanie
    \[\cos\theta_C = \frac{1}{n\beta}\]
    Rok
    1937
    Naukowiec
    Enrico Fermi, Wolfgang Pauli
    Dziedzina
    Forces & Fields

  • Nickela

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

  • Nocturna

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

  • Null Beacon

    Moc
    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.
    Równanie
    \[d_{\text{EH}}(t) = a(t)\int_{t}^{\infty} \frac{c\,dt^{\prime}}{a(t^{\prime})}\]
    Rok
    1956
    Dziedzina
    Relativity & Cosmos