As i suspected, your are ignorant of basic earth science...
i should be paid for teaching you science ( as I am indeed a qualified science teacher )
read and learn
"
If the Earth had no atmosphere, then the entire energy received from the sun would reach the surface undisturbed, to be
reflected from and/or
absorbed by it. As it stands, the
Earth's surface reflects part of the solar energy. This is what makes the part of the Earth lit by the sun visible from space (
Figure 8) in the same way that the moon and the other members of the solar system are visible to us, despite the fact that they lack an inner source of visible radiation. The most obvious aspect of
Figure 7 is the
brightness of the Earth's cloud cover. A significant part of the Earth's reflectivity can be attributed to clouds (this is but one reason why they are so important for the Earth's climate). In climate texts the reflectivity of a planet is referred to as the
albedo of the planet and is expressed as a fraction. The Albedo of Earth depends on the geographical location (can you tell from Figure 7 which has higher albedo, the land or the ocean?). On the average however, the
Earth's albedo is about 0.3. This fraction of incoming radiation is reflected back into space. The other 0.7 part of the incoming solar radiation is absorbed by our planet.
Effective temperature.
By absorbing the incoming solar radiation, the Earth warms up and its temperature rises. If the Earth would have had no atmosphere or ocean, as is the case for example on the moon, it would get very warm on the sunlit face of the planet and much colder than we experience presently, on the dark side (the little warmth on the dark side would come from the limited amount of heat stored in the ground from the previous daytime - this is, to some extent, what we experience in a cloud-free, land locked desert climate).
We have seen that
all heated objects must emit electromagnetic radiation, particularly so if they are surrounded by empty space. This radiation is referred to as
outgoing. As long as the incoming radiative flux is larger than the outgoing, the radiated object will continue to warm, and its temperature will continue to increase. This in turn will result in an increase in the outgoing radiation (according to the
Stefan-Boltzman law the outgoing radiation increases faster than the temperature). At some point the object will emit as much radiation as the amount incoming and a
radiative equilibrium (or balance) will be reached. Using what we have learned about radiative heat transfer and some geometric calculation we can calculate the
equilibrium temperature of an object if we know the amount of incoming energy. Here is how we do that in the case of a planet rotating around the Sun:
First let us denote the solar radiative flux at the top of the planets atmosphere by
S (for solar constant) and the albedo of the planet by
A. Then let us figure out the total amount of radiation absorbed by the planet. To overcome the difficulty posed by the fact that the planets are spherical and their surface tilts with respect to the incoming radiation, note that the amount distributed over the sphere is equal the amount that would be collected on the planets surface if it was a disk (with the same radius as the sphere), placed perpendicular to the sunlight. If the planet's radius is
R the area of that disk is
πR2. Thus:
heat absorbed by planet = (1 - A) πR2S
The total heat radiated from the planet is equal to the energy flux implied by its temperature (from the Stefan-Boltzman law) times the entire surface of the planet or:
heat radiated from planet = (4πR2) σT4
In radiative balance we thus have:
(4πR2 ) σT4 = (1 - A) πR2S
Solving this equation for temperature we obtain:
Te = [(1-A)S / 4σ] 1/4
We have added a subscript
e to the temperature to emphasize that this would be the temperature of the planet if it had no atmosphere. It is referred to as the
effective temperature of the planet. According to this calculation, the effective temperature of Earth is about 255 K (or -18 °C). With this temperature the Earth radiation will be centered on a wavelength of about 11 μm, well within the range of infrared (IR) radiation.
Because of the spectral properties of the Sun and Earth radiation we tend to refer to them as "
shortwave" and "
longwave" radiation, respectively.