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  2. 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.

  3. 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 ...

  4. Theta wave - Wikipedia

    en.wikipedia.org/wiki/Theta_wave

    Theta waves generate the theta rhythm, a neural oscillation in the brain that underlies various aspects of cognition and behavior, including learning, memory, and spatial navigation in many animals. [ 1 ] [ 2 ] It can be recorded using various electrophysiological methods, such as electroencephalogram (EEG), recorded either from inside the ...

  5. 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

  6. Kerr–Newman metric - Wikipedia

    en.wikipedia.org/wiki/Kerr–Newman_metric

    The Kerr–Newman metric describes the spacetime geometry around a mass which is electrically charged and rotating. It is a vacuum solution which generalizes the Kerr metric (which describes an uncharged, rotating mass) by additionally taking into account the energy of an electromagnetic field, making it the most general asymptotically flat and stationary solution of the Einstein–Maxwell ...

  7. Maxwell's equations - Wikipedia

    en.wikipedia.org/wiki/Maxwell's_equations

    In the differential form formulation on arbitrary space times, F = ⁠ 1 / 2 ⁠ F αβ ‍ dx α ∧ dx β is the electromagnetic tensor considered as a 2-form, A = A α dx α is the potential 1-form, = is the current 3-form, d is the exterior derivative, and is the Hodge star on forms defined (up to its orientation, i.e. its sign) by the ...

  8. Schwarzschild geodesics - Wikipedia

    en.wikipedia.org/wiki/Schwarzschild_geodesics

    For example, the Schwarzschild radius of the Earth is roughly 9 mm (3 ⁄ 8 inch); at the surface of the Earth, the corrections to Newtonian gravity are only one part in a billion. The Schwarzschild radius of the Sun is much larger, roughly 2953 meters, but at its surface, the ratio r s r {\textstyle {\frac {r_{\text{s}}}{r}}} is roughly 4 ...

  9. 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.