Auringon sähkömagneettisesta säteilystä

The earth is 12,756 km in diameter at a distance of 149.6 million km from the sun.
So the earth subtends 12756/149600000 = 8.53 *10^-5 radians (linear) or
2.28 *10^-8 square radians (areal) as viewed from the sun.
The total area of a sphere is 4*pi*r^2 = 12.6 radians,
so the ratio of the visible size of the earth to the total size of the "sky" as viewed from the sun is 2.87 *10^-7 : 1.
So the earth gets about .0000287 percent of total energy of the sun falling on it.
Since the albedo of the earth is about .3, it directly reflects about 30% of this energy,
so the amount that "ends up on earth" (temporarily) is about .00002 percent, 1/50,000 of a percent.The shadow cast by the Earth is a disc with this radius so disc with area
W = 1368 W/m2 * (6371 km)^2 * pi = 1.744*10^17 Watts.The Earth's albedo is 0.367 that means 1–0.367 = 0.633 is absorbed by the Earth and 0.367 of the total is reflected away.
So 0.633*1.744*10^17 = 1.10422*10^17 Watts reaches the Earth.Kulmaläpimitta eli näennäinen koko (angular size)
Kulmaläpimitta kertoo kuinka suurena jokin esine tai kohde havaitsijalle näkyy eli näennäisen koon.
Jotta todellinen koko voidaan määritellä laskennallisesti, on tiedettävä kohteen etäisyys.
Auringon ja Kuun kulmaläpimitta on Maasta katsottuna noin 1900 kaarisekuntia eli puoli astetta.
Aurinko on 400 kertaa Kuuta suurempi, mutta 400 kertaa Kuuta kauempana Maasta, joten Maasta katsottuna Auringolla ja Kuulla on täsmälleen sama kulmaläpimitta.
1 aste on 60 kaariminuuttia tai toisin merkittynä 1° = 60′. Edelleen 1′ = 60 kaarisekuntia eli 60″.
Sun angular diameterAngular size
Solid angle of the sun is
So the radius is 1/4°Sun angular diameter: mean 0.5332°, range 0.5242°--0.5422°.
Moon angular diameter: mean 0.5286°, range 0.4889°--0.5683°.

The center of the sun, the core of the sun, which converts that hydrogen to helium, operates at a temperature of 100 million Kelvin. That's 10 to the 8 Kelvin.
Then what happens is that very hot core transmits that energy through a combination of radiation, electromagnetic radiation, thermal motion,
the very large overturning structure that's intrinsic to the sun. And finally, it delivers that to the outer photosphere.
The temperature drops from 10 million Kelvin in the core of the sun to 5,800 Kelvin at the photosphere of the sun (which is the the outer defining membrane of the sun).
4.4 x 10^16 wattsSaapuvasta säteilystä heijastuu ja siroaa 6% takaisin avaruuteen.
Heijastuminen tarkoittaa että säteily vain ikään kuin kimpoaa aineesta osumiskulman ja kappaleen pinnan suunnan ja aineen määrittämään suuntaan.
Sironta tarkoittaa sitä että aine absorboi säteilyn ja sen jälkeen emittoi säteilyn johonkin suuntaan jota on paljon vaikeampi mallintaa kuin heijastumista.
Pilvistä heijastuu noin 20 %
Maan pinnasta heijastuu noin 4%Ilma absorboi tästä säteilystäIlma pystyy kantamaan tietyn määrän energiaa riippuen sen ominaislämpökapasiteetista.https://www.nasa.gov/wp-content/uploads/2015/03/135642main_balance_trifold21.pdf
Averaged over an entire year, approximately 342 watts of solar energy fall upon every square meter of Earth.
This is a tremendous amount of energy — 44 quadrillion (4.4*10^16) watts of power to be exact.
At the same time the Sun's energy heats the planet, the planet radiates energy that we can't see with our eyes (longwave radiation or heat) back to space.
As an object heats up, it starts to dramatically increase the amount of heat energy it gives off.
So the more Earth heats up, the more rapidly it will lose energy to space.
https://www.nasa.gov/wp-content/uploads/2015/03/135642main_balance_trifold21.pdf
If we measure the total amount of energy Earth receives from the Sun and then subtract the total amount of energy Earth reflects and emits back to space,
we arrive at a number called an energy budget.
Over time, Earth's climate system tends toward an energy balance between incoming solar energy and outgoing thermal energy (heat).
If more solar energy comes in, then Earth warms and will emit more heat to space to restore the balance.*Not all of the Sun's energy that enters Earth's atmosphere makes it to the surface.
The atmosphere reflects some of the incoming solar energy back to space immediately
and absorbs still more energy before it can reach the surface.
The remaining energy strikes Earth and warms the surface.
The surface of the Sun has a temperature of about 5,800 Kelvin
At that temperature, most of the energy the Sun radiates is visible and near-infrared light. At Earth's average distance from the Sun (about 150 million kilometers), the average intensity of solar energy reaching the top of the atmosphere directly facing the Sun is about 1,360 watts per square meter
according to measurements made by the most recent NASA satellite missions. This amount of power is known as the total solar irradiance.
Because the Earth is a sphere, only areas near the equator at midday come close to being perpendicular to the path of incoming light. Everywhere else, the light comes in at an angle. The progressive decrease in the angle of solar illumination with increasing latitude reduces the average solar irradiance by an additional one-half.
Averaged over the entire planet, the amount of sunlight arriving at the top of Earth's atmosphere is only one-fourth of the total solar irradiance, or approximately 340 watts per square meter.
Of the 340 watts per square meter of solar energy that falls on the Earth, 29% is reflected back into space, primarily by clouds, but also by other bright surfaces and the atmosphere itself. About 23% of incoming energy is absorbed in the atmosphere by atmospheric gases, dust, and other particles. The remaining 48% is absorbed at the surface.The Sun's surface temperature is 5,500° C, and its peak radiation is in visible wavelengths of light. Earth's effective temperature—the temperature it appears when viewed from space—is -20° C, and it radiates energy that peaks in thermal infrared wavelengths.
https://earthobservatory.nasa.gov/features/EnergyBalance
How does Earth's climate system distribute the energy that it receives?
The Earth is always tilted 23.5° away from perpindicular in the Sun's orbit plane. Because of this tilt, as Earth revolves around the Sun over the course of a year, the position of the North and South Poles changes relative to the Sun. Earth's Northern Hemishpere receives more sunlight during the months of June, July and August and grows warmer, while Earth's Southern Hemisphere receives less sunlight and grows colder. In December, January, and February, the position changes so that the Southern Hemisphere receives more sunlight than the Northern Hemisphere, and the seasons reverse. The Equator on the other hand stays in nearly the same position relative to the Sun throughout the year, so the tropics experience much less seasonal variation.
Given enough time and barring outside influences, Earth's climate system will naturally distribute heat evenly over Earth's surface. Winds and ocean currents help to achieve this balance. In the winter hemisphere, there is much more heat energy concentrated in the tropics than there is at the Pole. This imbalance in heating aids the formation of the intense mid-latitude storms we frequently see during winter. As these storms move across the planet they transport heat energy from surplus areas in the tropics to deficit areas in polar regions and effectively even out the distribution of energy over the planet.
By contrast, in the summer hemisphere, the difference in heating between the Pole and the tropics is not nearly so large. As a result, we don't see as
many intense mid-latitude storms during the summer months. The storms that do form during the summer tend to be weaker and more localized.