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  2. Density of states - Wikipedia

    en.wikipedia.org/wiki/Density_of_states

    The density of states related to volume V and N countable energy levels is defined as: = = (()). Because the smallest allowed change of momentum for a particle in a box of dimension and length is () = (/), the volume-related density of states for continuous energy levels is obtained in the limit as ():= (()), Here, is the spatial dimension of the considered system and the wave vector.

  3. List of states of matter - Wikipedia

    en.wikipedia.org/wiki/List_of_states_of_matter

    For up to 10 −35 seconds after the Big Bang, the energy density of the universe was so high that the four forces of nature – strong, weak, electromagnetic, and gravitational – are thought to have been unified into one single force. The state of matter at this time is unknown.

  4. Van Hove singularity - Wikipedia

    en.wikipedia.org/wiki/Van_Hove_singularity

    The density of states which appears in the Fermi's Golden Rule expression is then the joint density of states, which is the number of electronic states in the conduction and valence bands that are separated by a given photon energy.

  5. Charge carrier density - Wikipedia

    en.wikipedia.org/wiki/Charge_carrier_density

    The carrier density is usually obtained theoretically by integrating the density of states over the energy range of charge carriers in the material (e.g. integrating over the conduction band for electrons, integrating over the valence band for holes).

  6. Population inversion - Wikipedia

    en.wikipedia.org/wiki/Population_inversion

    Calculable is the ratio of the populations of the two states at room temperature (T ≈ 300 K) for an energy difference ΔE that corresponds to light of a frequency corresponding to visible light (ν ≈ 5 × 10 14 Hz). In this case ΔE = E 2 − E 1 ≈ 2.07 eV, and kT ≈ 0.026 eV.

  7. Fermi gas - Wikipedia

    en.wikipedia.org/wiki/Fermi_gas

    For such a power-law density of states, the grand potential integral evaluates exactly to: [12] (,,) = + (), where () is the complete Fermi–Dirac integral (related to the polylogarithm). From this grand potential and its derivatives, all thermodynamic quantities of interest can be recovered.

  8. Bose–Einstein condensate - Wikipedia

    en.wikipedia.org/wiki/Bose–Einstein_condensate

    In this limit, the gas is classical. As the density increases or the temperature decreases, the number of accessible states per particle becomes smaller, and at some point, more particles will be forced into a single state than the maximum allowed for that state by statistical weighting.

  9. Density - Wikipedia

    en.wikipedia.org/wiki/Density

    The Imperial gallon was based on the concept that an Imperial fluid ounce of water would have a mass of one Avoirdupois ounce, and indeed 1 g/cm 3 ≈ 1.00224129 ounces per Imperial fluid ounce = 10.0224129 pounds per Imperial gallon. The density of precious metals could conceivably be based on Troy ounces and pounds, a possible cause of confusion.