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  2. Flux - Wikipedia

    en.wikipedia.org/wiki/Flux

    Bottom: Field line through a curved surface, showing the setup of the unit normal and surface element to calculate flux. To calculate the flux of a vector field F (red arrows) through a surface S the surface is divided into small patches dS. The flux through each patch is equal to the normal (perpendicular) component of the field, the dot ...

  3. Radiant exposure - Wikipedia

    en.wikipedia.org/wiki/Radiant_exposure

    Radiant flux per unit frequency or wavelength. The latter is commonly measured in W⋅nm −1. Φ e,λ [nb 4] watt per metre W/m M⋅L⋅T −3: Radiant intensity: I e,Ω [nb 5] watt per steradian: W/sr: M⋅L 2 ⋅T −3: Radiant flux emitted, reflected, transmitted or received, per unit solid angle. This is a directional quantity. Spectral ...

  4. Spectral flux density - Wikipedia

    en.wikipedia.org/wiki/Spectral_flux_density

    The relative spectral flux density is also useful if we wish to compare a source's flux density at one wavelength with the same source's flux density at another wavelength; for example, if we wish to demonstrate how the Sun's spectrum peaks in the visible part of the EM spectrum, a graph of the Sun's relative spectral flux density will suffice.

  5. Jansky - Wikipedia

    en.wikipedia.org/wiki/Jansky

    To calculate the flux density in janskys, the total power detected (in watts) is divided by the receiver collecting area (in square meters), and then divided by the detector bandwidth (in hertz). The flux density of astronomical sources is many orders of magnitude below 1 W·m −2 ·Hz −1 , so the result is multiplied by 10 26 to get a more ...

  6. Intensity (physics) - Wikipedia

    en.wikipedia.org/wiki/Intensity_(physics)

    In physics and many other areas of science and engineering the intensity or flux of radiant energy is the power transferred per unit area, where the area is measured on the plane perpendicular to the direction of propagation of the energy. [a] In the SI system, it has units watts per square metre (W/m 2), or kg⋅s −3 in base units.

  7. Radiation pressure - Wikipedia

    en.wikipedia.org/wiki/Radiation_pressure

    The magnitude, denoted by S, divided by the speed of light is the density of the linear momentum per unit area (pressure) of the electromagnetic field. So, dimensionally, the Poynting vector is S = ⁠ power / area ⁠ = ⁠ rate of doing work / area ⁠ = ⁠ ⁠ ΔF / Δt ⁠ Δx / area ⁠, which is the speed of light, c = Δx / Δt, times ...

  8. Radiative flux - Wikipedia

    en.wikipedia.org/wiki/Radiative_flux

    In geophysics, shortwave flux is a result of specular and diffuse reflection of incident shortwave radiation by the underlying surface. [3] This shortwave radiation, as solar radiation, can have a profound impact on certain biophysical processes of vegetation, such as canopy photosynthesis and land surface energy budgets, by being absorbed into the soil and canopies. [4]

  9. Luminosity distance - Wikipedia

    en.wikipedia.org/wiki/Luminosity_distance

    Luminosity distance D L is defined in terms of the relationship between the absolute magnitude M and apparent magnitude m of an astronomical object. = ⁡ which gives: = + where D L is measured in parsecs.