⚙ Tinkers Space
❀ ✿

Quantum Mechanics & Physics

The theories and equations that describe reality — from the smallest particles to the curve of spacetime itself. A working reference for the curious.

✿ ❀ ❀ ✿

⚛ Quantum Mechanics

Planck's Quantum Hypothesis

Max Planck, 1900 — the birth of quantum theory

Energy isn't continuous — it comes in discrete packets called quanta. This single idea, proposed to solve the blackbody radiation problem, cracked classical physics open.

E = hfEnergy of a quantum = Planck's constant × frequency
foundations

Wave-Particle Duality

Louis de Broglie, 1924 · confirmed by Davisson–Germer, 1927

Everything — light, electrons, even you — behaves as both a wave and a particle. Matter has a wavelength, inversely proportional to its momentum.

λ = h / pde Broglie wavelength = Planck's constant ÷ momentum
foundations

The Schrödinger Equation

Erwin Schrödinger, 1926

The central equation of quantum mechanics. It describes how the quantum state of a system — the wavefunction ψ — evolves over time. The wavefunction encodes everything knowable about a particle.

iℏ ∂ψ/∂t = ĤψTime-dependent Schrödinger equation
Ĥψ = EψTime-independent form — the allowed energy states
core equation

Heisenberg Uncertainty Principle

Werner Heisenberg, 1927

You cannot simultaneously know a particle's exact position and exact momentum. This isn't a measurement limitation — it's how reality is built.

Δx · Δp ≥ ℏ/2Position uncertainty × momentum uncertainty
ΔE · Δt ≥ ℏ/2Energy–time version — virtual particles borrow energy briefly
core principle

Superposition & the Born Rule

Max Born, 1926

A quantum system exists in all possible states at once until measured. The wavefunction's squared amplitude gives the probability of finding each outcome — the universe runs on probability at its core.

|ψ⟩ = α|0⟩ + β|1⟩A qubit in superposition — both states, weighted by α and β
P = |ψ|²Born rule: probability = squared amplitude
core principle

Quantum Entanglement

Einstein, Podolsky & Rosen, 1935 · Bell, 1964

Two particles can share a single quantum state — measure one, and the other responds instantly, no matter the distance. Einstein called it "spooky action at a distance." Bell's theorem proved it's real.

|Φ⁺⟩ = (|00⟩ + |11⟩) / √2Bell state — maximally entangled pair
entanglement

Pauli Exclusion Principle

Wolfgang Pauli, 1925

No two fermions (electrons, protons, neutrons) can occupy the same quantum state simultaneously. This is why atoms have structure, why matter is solid, why chemistry exists.

No identical fermions share all four quantum numbers(n, l, ml, ms)
core principle

Quantum Tunneling

George Gamow, 1928

Particles can pass through energy barriers they classically shouldn't be able to cross. The wavefunction leaks through. This powers the sun, enables scanning tunneling microscopes — and flash memory.

T ≈ e−2κLTransmission probability decays exponentially with barrier width
phenomenon

The Dirac Equation

Paul Dirac, 1928

Quantum mechanics meets special relativity. Dirac's equation describes relativistic electrons — and predicted the existence of antimatter before it was ever observed.

(iℏγμ∂μ − mc)ψ = 0Relativistic wave equation for fermions
relativistic QM

Quantum Harmonic Oscillator

Foundational model across physics

The quantum version of a mass on a spring. Its evenly-spaced energy levels underpin quantum field theory — every particle is an excitation of its field, modeled as oscillators.

En = ℏω(n + ½)Energy levels — note the zero-point energy ℏω/2
foundations

🌌 Relativity & Cosmology

Mass–Energy Equivalence

Albert Einstein, 1905

Mass and energy are the same thing in different forms. A small amount of mass holds an enormous amount of energy — the principle behind nuclear power and the sun.

E = mc²Energy = mass × speed of light squared
special relativity

General Relativity — Field Equations

Albert Einstein, 1915

Gravity isn't a force — it's the curvature of spacetime caused by mass and energy. These ten equations describe how matter tells spacetime how to curve, and curved spacetime tells matter how to move.

Gμν + Λgμν = (8πG/c⁴) TμνEinstein field equations
general relativity

Time Dilation & Length Contraction

Special relativity, 1905

Time slows down and lengths contract for objects moving near light speed, relative to a stationary observer. GPS satellites must correct for this daily.

Δt' = Δt / √(1 − v²/c²)Moving clocks tick slower (Lorentz factor)
special relativity

🧲 Electromagnetism

Maxwell's Equations

James Clerk Maxwell, 1860s

Four equations that unified electricity, magnetism, and light. They predicted electromagnetic waves traveling at the speed of light — revealing that light is an electromagnetic wave.

∇·E = ρ/ε₀Gauss's law — electric charges produce electric fields
∇·B = 0No magnetic monopoles — field lines always loop
∇×E = −∂B/∂tFaraday's law — changing magnetic fields create electric fields
∇×B = μ₀J + μ₀ε₀∂E/∂tAmpère–Maxwell law — currents and changing E-fields create B-fields
classical

Lorentz Force

Hendrik Lorentz

The force on a charged particle moving through electric and magnetic fields — the basis of motors, particle accelerators, and mass spectrometers.

F = q(E + v × B)Force = charge × (electric field + velocity cross magnetic field)
classical

🔥 Thermodynamics

The Four Laws

19th century — Clausius, Kelvin, and others

Zeroth: If A = B and B = C in thermal equilibrium, then A = C. Defines temperature.
First: Energy is conserved — ΔU = Q − W.
Second: Entropy always increases — S ≥ 0. Time's arrow.
Third: Absolute zero is unreachable.

ΔS ≥ 0Second law — the universe trends toward disorder
classical

Statistical Mechanics — Boltzmann

Ludwig Boltzmann, 1870s

Connects the microscopic world of particles to macroscopic thermodynamics. Entropy is just counting microstates.

S = kB log WEntropy = Boltzmann constant × log of microstates
statistical

🍎 Classical Mechanics

Newton's Laws

Isaac Newton, 1687 — Principia

First: Objects in motion stay in motion unless acted upon.
Second: Force equals mass times acceleration.
Third: Every action has an equal and opposite reaction.

F = maThe second law — the workhorse of classical physics
classical

Universal Gravitation

Isaac Newton, 1687

Every mass attracts every other mass. Accurate enough to land rovers on Mars — superseded by general relativity only in extreme gravity.

F = G(m₁m₂)/r²Gravitational force between two masses
classical

Lagrangian & Hamiltonian Mechanics

Lagrange, 1788 · Hamilton, 1833

Reformulations of classical mechanics in terms of energy rather than forces. The Lagrangian (L = T − V) and Hamiltonian frameworks became the language of quantum mechanics and field theory.

d/dt(∂L/∂q̇) − ∂L/∂q = 0Euler–Lagrange equation
analytical

🪐 Orbital Mechanics

Kepler's Laws

Johannes Kepler, 1609–1619

First: Orbits are ellipses with the central body at one focus.
Second: A line from planet to sun sweeps equal areas in equal times.
Third: The square of the orbital period is proportional to the cube of the semi-major axis.

T² ∝ a³Kepler's third law — period vs. orbital radius
orbital

Vis-Viva Equation

The workhorse of orbital maneuvers

Gives the speed of a body in orbit at any point, given its distance from the central body and the orbit's semi-major axis. Essential for Hohmann transfers and rendezvous calculations.

v² = μ(2/r − 1/a)μ = gravitational parameter, r = distance, a = semi-major axis
orbital

Tsiolkovsky Rocket Equation

Konstantin Tsiolkovsky, 1903

The tyranny of the rocket equation: the velocity a rocket can achieve depends on exhaust speed and the ratio of initial to final mass. This is why staging exists.

Δv = ve ln(m₀/mf)Delta-v = exhaust velocity × ln(mass ratio)
orbital

🧬 The Standard Model

Particles & Forces

Developed 1960s–1970s · confirmed through 2012 (Higgs)

Our best description of fundamental particles and three of the four forces (electromagnetic, weak, strong — gravity excluded). Fermions (quarks, leptons) make up matter; bosons (photon, gluon, W/Z, Higgs) carry forces.

ℒ = −¼FμνFμν + iψ̄D̸ψ + …The Standard Model Lagrangian (abbreviated — the full form fills pages)
particle physics