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    • https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Planetary_Photometry_(Tatum_and_Fairbairn)/01%3A_Principles_of_Planetary_Photometry/1.02%3A_Radiance_and_the_Equation_of_Transfer
      projected on a plane at right angles to the line of sight from the observer); or it is the power arriving per unit area at the observer from unit solid angle (subtended at the observer) of the extende...projected on a plane at right angles to the line of sight from the observer); or it is the power arriving per unit area at the observer from unit solid angle (subtended at the observer) of the extended source. Here \(\frac{d L}{d s}\) is the rate of change of radiance with, and in the direction of, position \(s\) in a given medium, r is the density of the medium (kg m -3 ) and \(κ\) is the mass attenuation coefficient (m 2 kg -1 ).

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