quantity

density of states

The number of available electronic states per energy interval in a material.
8 related articles · 3 formulas

Description

The density of states (DOS) is a fundamental quantity in solid-state physics that counts how many electronic states are available at each energy level. It is a function that peaks where many states exist (e.g., in flat bands) and vanishes in band gaps. The DOS determines how many electrons can occupy a given energy range and directly influences a material's electrical, thermal, and optical behavior.

How it works

In a crystal, electrons occupy discrete energy bands. The DOS is computed by counting, for each energy E, the number of quantum states with energy between E and E+dE. It depends on the dispersion relation (how energy varies with momentum). For example, in a 2D electron gas, the DOS is constant per unit area, while in 1D it has sharp peaks called van Hove singularities.

In practice

The DOS is essential for interpreting scanning tunneling spectroscopy, designing thermoelectric materials, and predicting the performance of transistors and quantum well lasers.

Fun fact

In graphene, the density of states vanishes linearly at the Dirac point, making it a zero-gap semiconductor with unusual electronic behavior.

Concept graph →

Formulas

$$\Gamma_{i\to f} = \frac{2\pi}{\hbar} |\langle \psi_f | H' | \psi_i \rangle|^2 \rho(E_f)$$
Transition rate due to perturbation depends on matrix element and density of states.
What is in the formula
\Gamma_{i\to f}variableTransition rate from initial state i to final state f — transition rate per second
\psi_ivariableInitial quantum state — wave function
\psi_fvariableFinal quantum state — wave function
H'variablePerturbation Hamiltonian — perturbation hamiltonian joule
\rho(E_f)variableDensity of final states at energy E_f — density of states per joule
\hbarconstantReduced Planck constant, relating energy to angular frequency — reduced planck constant = 1.054571817e-34 joule second
\langle \psi_f | H' operatorMatrix element of the perturbation between initial and final states — matrix element
$$J(E) = \frac{2}{(2\pi)^3} \int_{\text{BZ}} d^3k \, \delta(E_c(\mathbf{k}) - E_v(\mathbf{k}) - E)$$
Number of electronic transitions per energy interval.
What is in the formula
Jvariablejoint density of states — density of states per joule per cubic metre
Evariablephoton energy — energy joule
E_cvariableconduction band energy — energy joule
E_vvariablevalence band energy — energy joule
\mathbf{k}variablecrystal momentum — wave vector per metre
\int_{\text{BZ}} d^3operatorintegration over the first Brillouin zone — integral over brillouin zone
\deltaoperatorselects states satisfying energy conservation — dirac delta function
$$g(\omega) \propto \frac{\omega^3}{e^{\hbar\omega/kT} - 1}$$
Describes the universal low-frequency scaling of vibrational modes in glasses.
What is in the formula
g(ω)variablevibrational density of states — density of states second per radian
ωvariableangular frequency — angular frequency radian per second
Tvariabletemperature — temperature kelvin
ħconstantReduced Planck constant, quantum of angular momentum — reduced planck constant = 1.054571817e-34 joule second
kconstantRelates energy to temperature in statistical mechanics — boltzmann constant = 1.380649e-23 joule per kelvin

Related articles · 8

General Relativity2026-08-062 minarXiv:2608.05794express
The Tidal Fingerprint of Neutron Stars
The merger of two neutron stars is not just a collision. Even before they touch, they deform each other through tidal forces, and this deformation depends on how 'soft' or 'stiff' the matter inside is. Stiff matter resists more; soft matter changes shape more easily.
The Voice of a Neutron Star: The Song of Superdense Matter
In 2017, the LIGO and Virgo detectors recorded the spacetime tremor from the collision of two neutron star merger — event GW170817. After the initial burst came an after-ring: a kilohertz oscillation of the newly formed superdense remnant.
Quantum Physics2026-06-172 minarXiv:2606.19649express
Quantum Whisper: Squeezed Light Yields to New States
Gravitational-wave observatories are like a keen ear listening for distant rumbles of cosmic catastrophes. To catch the faint whisper of merging black holes, detectors of gravitational waves use specially prepared light — known as squeezed vacuum.
Quantum Physics2026-06-161 minarXiv:2606.18348express
A Kiss of Spectra: How a Dance of Energy Survives Friction
The quantum world is full of surprises. In a Kerr parametric oscillator, a device where light is trapped in a ring and driven by an external field, researchers recently noticed something strange: pairs of energy levels merge in an embrace. Physicists have dubbed this a "spectral kiss" spectroscopy.
The Quark Symphony of a Neutron Star
The core of a neutron star can be likened to a taut string of super-nuclear density. Sound traveling along it is the oscillation of pressure, whose speed $$c_s$$ betrays the stiffness of matter. New research shows that this cosmic string does not hum monotonically.
Materials2026-04-232 minarXiv:2604.21283express
Hidden Voids in Metal
A copper wire under current is a familiar sight, but inside it something unexpected is happening. A strong electric current doesn't just heat the metal: it knocks atoms out of their rightful places, leaving behind tiny voids, as if a few balls were suddenly removed from a tightly packed arrangement.
Atomic Physics2026-03-102 minarXiv:2603.09102express
Two Electrons, One Laser Strike
A laser strikes a strontium atom, and two electrons fly out at once. Previously, it was thought that in such double ionization each electron acts on its own: one is knocked out first, the second later, randomly.
Nuclear Theory2026-01-061 minarXiv:2601.02980express
The Ultimate Stiffness Limit of Neutron Stars
Just as in a crowded room each new person sharply increases the pressure on the walls, in a neutron star increasing density leads to a rise in internal resistance. But even this resistance has an absolute ceiling.