--%>
Assignment Help - homework help

Explain Stefan-Boltzmann law

Stefan-Boltzmann law (Stefan, L. Boltzmann): The radiated power P (that is the rate of emission of electromagnetic energy) of a hot body is proportional to the radiating surface area, A, and the 4th power of the thermodynamic temperature, T. The constant of proportionality is Stefan-Boltzmann constant. Scientifically,

P = e sigma A T4,

Here the efficiency rating e is termed as the emissivity of the object.

   Related Questions in Physics

  • Q : Define Landauers principle Landauer's

    Landauer's principle: The principle which defines that it doesn't explicitly take energy to calculate data, however instead it takes energy to remove any data, as erasure is a vital step in computation.

    		•
  • Q : What is Lyman series Lyman series: The

    Lyman series: The sequence that explains the emission spectrum of hydrogen whenever electrons are jumping to the ground state. Each and every line is in the ultraviolet.

    		•
  • Q : Define Weiss constant Weiss constant :

    Weiss constant: The characteristic constant dependent on the substance, employed in computing the susceptibility of the paramagnetic materials.

    		•
  • Q : What is Permeability of free space or

    Permeability of free space: magnetic constant: mu_0: The ratio of the magnetic flux density in the substance to the external field strength for vacuum. It is equivalent to 4 pi x 10-7 H/m.

    		•
  • Q : Define Dirac constant Dirac constant :

    Dirac constant: Planck constant, modified form; hbar Sometimes more suitable form of the Planck constant, stated as: hbar = h/(2 pi)

    		•
  • Q : What is Paschen series Paschen series:

    Paschen series: The series that explains the emission spectrum of hydrogen whenever the electron is jumping to the third orbital. Each and every line is in the infrared part of the spectrum.

    		•
  • Q : What is Chandrasekhar limit

    Chandrasekhar limit (S. Chandrasekhar; 1930): A limit that mandates that no white dwarf (a collapsed, degenerate star) can be much massive than around 1.4 masses solar. Any of the degenerate mass more massive should inevitably collaps

    		•
  • Q : Newtons laws of motion Briefly

    Briefly illustrate all the Newton s laws of motion?

    		•
  • Q : Define Static limit Static limit : The

    Static limit: The distance from a rotating black hole where no spectator can possibly stay at rest (with respect to the far-away stars) since of inertial frame dragging; this area is external of the event horizon, apart from at the poles where it meet

    		•
  • Q : Define Rydberg constant Rydberg

    Rydberg constant (Rydberg): The constant that governs the relationship of the spectral line features of an atom via the Rydberg formula. For hydrogen, it is around 1.097 x 107 m-1.

    		•