This radiant energy arrives at the Earth in a broad band of electromagnetic spectra . The Earth and Suns' radiation spectrum follow two important laws, the Stefan-Boltzmann law and Wien's law . K. Wien's law explains why the Sun, with at temperature of 6000K emits its maximum energy at a wavelength of about 0.5 m m while the Earth with a mean temperature of about 285K emits its maximum energy at about 10um. This means that hot bodies not only radiate more energy, they radiate at shorter wave lengths. The law of the conservation of energy requires that we account for all of the energy received by the Earth.
Energy is conserved.
We can use the conservation of energy to calculate the Earth's planetary temperature. In this equation, R 2 p and 4R 2 p represent the area of a sphere and the area of a disk. The Earth's area that receives solar radiation at any given time turns out to have the shape of a disk. Some of the energy Earth receives from the Sun in the form of electromagnetic energy pass undisturbed, some are absorbed by the atmosphere, and the rest are turned back. Oxygen, ozone, water vapor, carbon dioxide and dust are the most important absorbers of shortwave length energy from the Sun and longwave radiation emitted by by the Earth.