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 {| border="1" cellpadding="5" cellspacing="0"
 * + style="caption-side: bottom" | Fig. 4.1
 * align="center" width="50%" | Gas || align="center" width="50%" | Volume
 * Nitrogen (N$2)$ || 780,840 ppmv (78.084%)
 * Oxygen (O$2)$ || 209,460 ppmv (20.946%)
 * Argon (Ar) || 9,340 ppmv (0.9340%)
 * Carbon dioxide (CO$2)$ || 393.65 ppmv (0.039365%)
 * Neon (Ne) || 18.18 ppmv (0.001818%)
 * Methane (CH$4$) || 1.77 ppmv (0.000177%)
 * Helium (He) || 5.24 ppmv (0.000524%)
 * Krypton (Kr) || 1.14 ppmv (0.000114%)
 * Hydrogen (H$2$) || 0.55 ppmv (0.000055%)
 * Nitrous oxide (N$2$O) || 0.3 ppmv (0.00003%)
 * Carbon monoxide (CO) || 0.1 ppmv (0.00001%)
 * Xenon (Xe) || 0.09 ppmv (0.000009%)
 * Ozone (O$3$) || 0.0 to 0.07 ppmv (0 to 0.000007%)
 * Nitrogen dioxide (NO$2$) || 0.02 ppmv (0.000002%)
 * Iodine (I$2$) || 0.01 ppmv (0.000001%)
 * Ammonia (NH$3$) || trace
 * Water vapor (H$2$O) || ~0.40% over full atmosphere, typically 1%-4% at surface
 * }
 * Hydrogen (H⇭⇭⇭) || 0.55 ppmv (0.000055%)
 * Nitrous oxide (N⇭⇭⇭O) || 0.3 ppmv (0.00003%)
 * Carbon monoxide (CO) || 0.1 ppmv (0.00001%)
 * Xenon (Xe) || 0.09 ppmv (0.000009%)
 * Ozone (O⇭⇭⇭) || 0.0 to 0.07 ppmv (0 to 0.000007%)
 * Nitrogen dioxide (NO⇭⇭⇭) || 0.02 ppmv (0.000002%)
 * Iodine (I⇭⇭⇭) || 0.01 ppmv (0.000001%)
 * Ammonia (NH⇭⇭⇭) || trace
 * Water vapor (H⇭⇭⇭O) || ~0.40% over full atmosphere, typically 1%-4% at surface
 * }
 * Nitrogen dioxide (NO⇭⇭⇭) || 0.02 ppmv (0.000002%)
 * Iodine (I⇭⇭⇭) || 0.01 ppmv (0.000001%)
 * Ammonia (NH⇭⇭⇭) || trace
 * Water vapor (H⇭⇭⇭O) || ~0.40% over full atmosphere, typically 1%-4% at surface
 * }
 * Water vapor (H⇭⇭⇭O) || ~0.40% over full atmosphere, typically 1%-4% at surface
 * }
 * }
 * }

Different gases have different absorption properties, and so interact differently with various wavelengths of radiation. Radiation of a given wavelength may pass almost unimpeded through relatively thick layers of one gas, but be almost totally absorbed by even small amounts of another gas. This is the source of the greenhouse effect: the composition of the atmosphere directly affects how much radiation (and of which wavelengths) is able to escape to space. Recall that the wavelength of the energy radiated by an object depends on its absolute

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