Quantum Physics
Pauli Exclusion Principle
No two fermions can occupy the same quantum state — why atoms have structure
The Pauli exclusion principle (1925) — no two fermions (half-integer spin particles) can occupy the same quantum state. Critical for atomic structure (electrons fill orbitals in pairs), chemistry (periodic table makes sense), white dwarfs and neutron stars (degeneracy pressure), and metallic conductivity (Fermi sea).
- StatementNo two identical fermions in same quantum state
- DiscoveredWolfgang Pauli, 1925
- Applies toHalf-integer spin particles (electrons, protons, neutrons, quarks)
- Doesn't apply toBosons (integer spin) — many can be in same state
- Atomic shellsEach shell has limited spots (2n²); electrons fill systematically
- Degeneracy pressureHolds up white dwarfs, neutron stars
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The principle
No two identical fermions can occupy the same quantum state simultaneously.
"Quantum state" specifies all quantum numbers: position/momentum, spin, energy, etc. For an electron in an atom — n (principal), ℓ (orbital), m_ℓ (magnetic), m_s (spin = ±½). Each state holds at most one electron.
Application to atoms
Electrons fill orbitals from bottom up:
| Shell n | Subshells | Max electrons |
|---|---|---|
| 1 | 1s (2) | 2 |
| 2 | 2s (2), 2p (6) | 8 |
| 3 | 3s (2), 3p (6), 3d (10) | 18 |
| 4 | 4s (2), 4p (6), 4d (10), 4f (14) | 32 |
| n general | Combine all | 2n² |
Filling order (Aufbau): 1s 2s 2p 3s 3p 4s 3d 4p 5s 4d 5p 6s 4f 5d 6p 7s 5f 6d 7p — based on energy levels.
Periodic table structure
| Row | Filling | Elements |
|---|---|---|
| 1 | 1s (2) | H, He |
| 2 | 2s, 2p (8) | Li-Ne |
| 3 | 3s, 3p (8) | Na-Ar |
| 4 | 4s, 3d, 4p (18) | K-Kr |
| 5 | 5s, 4d, 5p (18) | Rb-Xe |
| 6 | 6s, 4f, 5d, 6p (32) | Cs-Rn |
JavaScript — Pauli exclusion
// Maximum electrons in shell n
function maxElectrons(n) {
return 2 * n * n;
}
[1, 2, 3, 4, 5].forEach(n => {
console.log(`Shell n=${n}: max ${maxElectrons(n)} electrons`);
});
// Electron configuration of common elements
function electronConfig(Z) {
// Aufbau filling order (simplified)
const orbitals = [
{ name: '1s', max: 2 },
{ name: '2s', max: 2 },
{ name: '2p', max: 6 },
{ name: '3s', max: 2 },
{ name: '3p', max: 6 },
{ name: '4s', max: 2 },
{ name: '3d', max: 10 },
{ name: '4p', max: 6 },
{ name: '5s', max: 2 },
// ...etc
];
let remaining = Z;
const config = [];
for (const orbital of orbitals) {
if (remaining === 0) break;
const filled = Math.min(remaining, orbital.max);
config.push(`${orbital.name}^${filled}`);
remaining -= filled;
}
return config.join(' ');
}
// Hydrogen (Z=1): 1s¹
// Carbon (Z=6): 1s² 2s² 2p²
// Iron (Z=26): 1s² 2s² 2p⁶ 3s² 3p⁶ 4s² 3d⁶
console.log(`H: ${electronConfig(1)}`);
console.log(`C: ${electronConfig(6)}`);
console.log(`Ne: ${electronConfig(10)}`);
console.log(`Na: ${electronConfig(11)}`);
// White dwarf: degeneracy pressure
function chandrasekharLimit() {
// Mass limit for white dwarf supported by electron degeneracy pressure
return 1.4; // solar masses
}
console.log(`Chandrasekhar limit: ${chandrasekharLimit()} M_sun`);
// White dwarfs heavier than this collapse to neutron stars
// Density of state-filling
function fermiTemperature(electronDensity, m_electron = 9.11e-31) {
// T_F = E_F / k_B
// E_F ≈ ℏ²(3π²n)^(2/3) / (2m)
const h_bar = 1.055e-34;
const k_B = 1.38e-23;
const E_F = h_bar * h_bar * Math.pow(3 * Math.PI * Math.PI * electronDensity, 2/3) / (2 * m_electron);
return E_F / k_B;
}
// Free electrons in copper: ~8 × 10²⁸ /m³
console.log(`Copper Fermi T: ${fermiTemperature(8e28).toExponential(2)} K`);
// ~80,000 K — much higher than room T → electrons strongly degenerate
Where Pauli exclusion matters
- Atomic structure. All atoms with multiple electrons.
- Chemistry. Bonds, periodic table, every chemical reaction.
- Solid state physics. Metals, semiconductors, insulators — all rely on Pauli filling.
- Stars. White dwarf and neutron star structure; supernova mechanics.
- Quantum gases. Fermi gas of neutrons, electrons, atoms.
- Plasma. Hot dense plasmas show electron degeneracy.
- Quantum computing. Distinguish fermionic (electron) qubits from bosonic ones.
Common mistakes
- Applying Pauli to bosons. Bosons (photons, gluons, He-4) DON'T obey exclusion. Multiple bosons can share state.
- Treating spin as classical. Spin is intrinsic angular momentum, quantized in units of ℏ/2 for fermions. Two spin states (up/down) double available states.
- Confusing "different state" with "different position." Two electrons in same orbital can have different spins (different m_s) — counts as different states.
- Forgetting it's exact. Pauli is fundamental; not a probabilistic statement. Truly NEVER two identical fermions in same state.
- Thinking Pauli applies between non-identical particles. Different particle types are distinguishable; can share quantum numbers. Only identical fermions excluded.
- Confusing degeneracy with random arrangements. Degeneracy pressure (white dwarf) is from filling states — not "regular" pressure.
Frequently asked questions
Why can't two electrons be in the same state?
Mathematical fact about fermions. Their wave function must be ANTISYMMETRIC under exchange — swap two electrons and Ψ → -Ψ. If they were in the same state, Ψ would also = Ψ, requiring Ψ = 0 (impossible state). Result: at most one fermion per quantum state.
How does this give atoms their structure?
Electrons fill energy levels from bottom up, two per orbital (one with spin up, one down — different m_s quantum numbers). Hydrogen has 1 electron in 1s. Helium has 2 (fills 1s). Lithium 3 (fills 1s, starts 2s). Etc. The "shell" structure of atoms — and the periodic table — is direct consequence of Pauli exclusion. Without it, all electrons would crash into ground state and no chemistry.
How does Pauli explain white dwarfs?
Stars after H burning. Without thermonuclear power, gravity wants to collapse star. Electrons in dense plasma can't be pushed into already-occupied states (Pauli) — they have HUGE momentum (high quantum levels filled). This creates "electron degeneracy pressure" — supports the star against gravity. Stops working above Chandrasekhar limit (~1.4 M_sun) — collapses to neutron star.
What about neutron stars?
Even more compact (~10 km radius). Electrons captured by protons forming neutrons. Neutron degeneracy pressure (also Pauli) holds against gravity. Stops working above Tolman-Oppenheimer-Volkoff limit (~2-3 M_sun) — collapses to black hole.
Do bosons follow Pauli exclusion?
No. Bosons have integer spin (0, 1, 2). Multiple bosons CAN occupy same state. This is why lasers work (many photons coherent in same state) and why Bose-Einstein condensates exist (atoms condense into ground state). Quantum statistics — Bose-Einstein for bosons, Fermi-Dirac for fermions.
Why does the periodic table have specific row lengths?
Pauli exclusion! Each electron shell has limit: 1s (2 e), 2s+2p (8), 3s+3p (8), 3d+4s+4p (18), etc. Row 1 — 2 elements. Row 2 — 8. Row 3 — 8. Row 4 — 18. Numbers come directly from filling rules. Mendeleev (1869) noticed pattern; quantum mechanics (1920s) explained it.
Are there exceptions to Pauli?
Pauli is exact for IDENTICAL fermions. Different particles (e.g., proton + neutron) can be in "same" orbital because they're distinguishable. Excitations (like phonons in solids) are bosons; many can collect. Pauli applies to truly identical fermions in the same single-particle state.