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  2. Solar constant - Wikipedia

    en.wikipedia.org/wiki/Solar_constant

    This is because the solar constant is evaluated at a fixed distance of 1 Astronomical Unit (au) while the solar irradiance will be affected by the eccentricity of the Earth's orbit. Its distance to the Sun varies annually between 147.1·10 6 km at perihelion and 152.1·10 6 km at aphelion .

  3. Radiation pressure - Wikipedia

    en.wikipedia.org/wiki/Radiation_pressure

    Solar radiation pressure on objects near the Earth may be calculated using the Sun's irradiance at 1 AU, known as the solar constant, or G SC, whose value is set at 1361 W/m 2 as of 2011. [17] All stars have a spectral energy distribution that depends on their surface temperature. The distribution is approximately that of black-body radiation.

  4. Solar irradiance - Wikipedia

    en.wikipedia.org/wiki/Solar_irradiance

    The solar constant is a conventional measure of mean TSI at a distance of one astronomical unit (AU). Direct normal irradiance (DNI), or beam radiation, is measured at the surface of the Earth at a given location with a surface element perpendicular to the Sun direction.

  5. Sun - Wikipedia

    en.wikipedia.org/wiki/Sun

    The solar constant is equal to approximately 1,368 W/m 2 (watts per square meter) at a distance of one astronomical unit (AU) from the Sun (that is, at or near Earth's orbit). [99] Sunlight on the surface of Earth is attenuated by Earth's atmosphere , so that less power arrives at the surface (closer to 1,000 W/m 2 ) in clear conditions when ...

  6. Sunlight - Wikipedia

    en.wikipedia.org/wiki/Sunlight

    The solar constant is a measure of flux density, is the amount of incoming solar electromagnetic radiation per unit area that would be incident on a plane perpendicular to the rays, at a distance of one astronomical unit (AU) (roughly the mean distance from the Sun to Earth). The "solar constant" includes all types of solar radiation, not just ...

  7. Stefan–Boltzmann law - Wikipedia

    en.wikipedia.org/wiki/Stefan–Boltzmann_law

    (Above the atmosphere, the result is even higher: 394 K (121 °C; 250 °F).) We can think of the earth's surface as "trying" to reach equilibrium temperature during the day, but being cooled by the atmosphere, and "trying" to reach equilibrium with starlight and possibly moonlight at night, but being warmed by the atmosphere.

  8. Air mass (solar energy) - Wikipedia

    en.wikipedia.org/wiki/Air_mass_(solar_energy)

    The earth's atmosphere absorbs a considerable amount of the ultraviolet light. The resulting spectrum at the Earth's surface has fewer photons, but they are of lower energy on average, so the number of photons, above the bandgap, per unit of sunlight energy is greater than in space. This means that solar cells are more efficient at AM1 than AM0.

  9. Earth's energy budget - Wikipedia

    en.wikipedia.org/wiki/Earth's_energy_budget

    This corresponds to an average flux of 0.087 W/m 2 and represents only 0.027% of Earth's total energy budget at the surface, being dwarfed by the 173 000 TW of incoming solar radiation. [ 13 ] Human production of energy is even lower at an average 18 TW, corresponding to an estimated 160,000 TW-hr, for all of year 2019. [ 14 ]