--%>

Explain Gauss law for magnetic fields

Gauss' law for magnetic fields (K.F. Gauss): The magnetic flux via a closed surface is zero (0); no magnetic charges present; in its differential form,

div B = 0

   Related Questions in Physics

  • Q : Meaning of Network Define the meaning

    Define the meaning of Network in brief.

  • Q : Bragg's law Bragg's law - Whenever a

    Bragg's law - Whenever a beam of x-rays strikes a crystal surface in which the layers of ions or atoms are often separated, the maximum intensity of the reflected ray takes place when the complement of the angle of incidence, theta (θ), the wave

  • Q : On which gravitational force depends

    Explain in short on which the gravitational force depends on?

  • Q : Explain Tachyon Tachyon: The purely

    Tachyon: The purely speculative particle that is supposed to travel faster than light. According to Sir Einstein's equations of special relativity, a particle with imaginary rest mass and a velocity more than c would contain a real momentum and energy

  • 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.

  • Q : Difference between the cathode ray and

    Illustrate the difference between the cathode ray and beta ray?

  • 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 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 : What is Hawking temperature Hawking

    Hawking temperature: The temperature of a black hole is caused by the emission of the hawking radiation. For a black hole with mass m, it is illustrated as: T = (hbar c3)/(8 pi G k m).

  • 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