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  2. Stefan–Boltzmann law - Wikipedia

    en.wikipedia.org/wiki/Stefan–Boltzmann_law

    The temperature Stefan obtained was a median value of previous ones, 1950 °C and the absolute thermodynamic one 2200 K. As 2.57 4 = 43.5, it follows from the law that the temperature of the Sun is 2.57 times greater than the temperature of the lamella, so Stefan got a value of 5430 °C or 5700 K. This was the first sensible value for the ...

  3. Mikheyev–Smirnov–Wolfenstein effect - Wikipedia

    en.wikipedia.org/wiki/Mikheyev–Smirnov...

    In the case of normal neutrino mass hierarchy, and ,, transitions occurred inside the star, then and oscillated inside the Earth. Due to the differences in the distance traveled by neutrinos to Kamiokande, IMB and Baksan within the Earth, the MSW effect can partially explain the difference of the Kamiokande and IMB energy spectrum of events.

  4. List of equations in wave theory - Wikipedia

    en.wikipedia.org/wiki/List_of_equations_in_wave...

    Position of a point in space, not necessarily a point on the wave profile or any line of propagation d, r: m [L] Wave profile displacement Along propagation direction, distance travelled (path length) by one wave from the source point r 0 to any point in space d (for longitudinal or transverse waves) L, d, r

  5. Geopotential spherical harmonic model - Wikipedia

    en.wikipedia.org/wiki/Geopotential_spherical...

    As P 0 n (x) = −P 0 n (−x) non-zero coefficients J n for odd n correspond to a lack of symmetry "north–south" relative the equatorial plane for the mass distribution of Earth. Non-zero coefficients C n m, S n m correspond to a lack of rotational symmetry around the polar axis for the mass distribution of Earth, i.e. to a "tri-axiality" of ...

  6. Radiation pressure - Wikipedia

    en.wikipedia.org/wiki/Radiation_pressure

    The above treatment for an incident wave accounts for the radiation pressure experienced by a black (totally absorbing) body. If the wave is specularly reflected, then the recoil due to the reflected wave will further contribute to the radiation pressure. In the case of a perfect reflector, this pressure will be identical to the pressure caused ...

  7. Scattering amplitude - Wikipedia

    en.wikipedia.org/wiki/Scattering_amplitude

    In quantum physics, the scattering amplitude is the probability amplitude of the outgoing spherical wave relative to the incoming plane wave in a stationary-state scattering process. [1] At large distances from the centrally symmetric scattering center, the plane wave is described by the wavefunction [ 2 ]

  8. Cavendish experiment - Wikipedia

    en.wikipedia.org/wiki/Cavendish_experiment

    Since there are two balls, each experiencing force F at a distance ⁠ L / 2 ⁠ from the axis of the balance, the torque due to gravitational force is LF. At equilibrium (when the balance has been stabilized at an angle θ {\displaystyle \theta } ), the total amount of torque must be zero as these two sources of torque balance out.

  9. Coriolis frequency - Wikipedia

    en.wikipedia.org/wiki/Coriolis_frequency

    Replacing =, where is the magnitude of the spin rate of the Earth, to obtain f = ω = 2 Ω sin ⁡ φ . {\displaystyle f=\omega =2\Omega \sin \varphi .} Thus the Coriolis parameter, f {\displaystyle f} , is the angular velocity or frequency required to maintain a body at a fixed circle of latitude or zonal region.