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  2. Logarithmic mean temperature difference - Wikipedia

    en.wikipedia.org/wiki/Logarithmic_mean...

    When the two temperature differences are equal, this formula does not directly resolve, so the LMTD is conventionally taken to equal its limit value, which is in this case trivially equal to the two differences. With this definition, the LMTD can be used to find the exchanged heat in a heat exchanger:

  3. Stefan–Boltzmann law - Wikipedia

    en.wikipedia.org/wiki/Stefan–Boltzmann_law

    The Stefan–Boltzmann law may be expressed as a formula for radiance as a function of temperature. Radiance is measured in watts per square metre per steradian (W⋅m −2 ⋅sr −1 ). The Stefan–Boltzmann law for the radiance of a black body is: [ 9 ] : 26 [ 10 ] L Ω âˆ˜ = M ∘ π = σ π T 4 . {\displaystyle L_{\Omega }^{\circ }={\frac ...

  4. NTU method - Wikipedia

    en.wikipedia.org/wiki/NTU_Method

    The number of transfer units (NTU) method is used to calculate the rate of heat transfer in heat exchangers (especially parallel flow, counter current, and cross-flow exchangers) when there is insufficient information to calculate the log mean temperature difference (LMTD). Alternatively, this method is useful for determining the expected heat ...

  5. List of electromagnetism equations - Wikipedia

    en.wikipedia.org/wiki/List_of_electromagnetism...

    Continuous charge distribution. The volume charge density ρ is the amount of charge per unit volume (cube), surface charge density σ is amount per unit surface area (circle) with outward unit normal nĖ‚, d is the dipole moment between two point charges, the volume density of these is the polarization density P.

  6. Boltzmann constant - Wikipedia

    en.wikipedia.org/wiki/Boltzmann_constant

    Boltzmann's grave in the Zentralfriedhof, Vienna, with bust and entropy formula. In statistical mechanics, the entropy S of an isolated system at thermodynamic equilibrium is defined as the natural logarithm of W , the number of distinct microscopic states available to the system given the macroscopic constraints (such as a fixed total energy E ...

  7. Black-body radiation - Wikipedia

    en.wikipedia.org/wiki/Black-body_radiation

    The law was formulated by Josef Stefan in 1879 and later derived by Ludwig Boltzmann. The formula E = σT 4 is given, where E is the radiant heat emitted from a unit of area per unit time, T is the absolute temperature, and σ = 5.670 367 × 10 −8 W·m −2 ⋅K −4 is the Stefan–Boltzmann constant. [28]

  8. Boltzmann equation - Wikipedia

    en.wikipedia.org/wiki/Boltzmann_equation

    The general equation can then be written as [6] = + + (),. where the "force" term corresponds to the forces exerted on the particles by an external influence (not by the particles themselves), the "diff" term represents the diffusion of particles, and "coll" is the collision term – accounting for the forces acting between particles in collisions.

  9. Heat transfer coefficient - Wikipedia

    en.wikipedia.org/wiki/Heat_transfer_coefficient

    Although convective heat transfer can be derived analytically through dimensional analysis, exact analysis of the boundary layer, approximate integral analysis of the boundary layer and analogies between energy and momentum transfer, these analytic approaches may not offer practical solutions to all problems when there are no mathematical models applicable.