The planetary temperature energy balance is obtained by radiating back the absorbed radiation energy from outer-space, by the planet and thus acquiring thermal equilibrium.
What is the process of attaining thermal equilibrium by Earth?
The Stefan-Boltzmann law states that the more the temperature a planet has, the more it will radiate out to reach thermal equilibrium.
We know that outer space contains large masses of radiative energy freely distributed in its vast expanse. A small fraction of this energy is absorbed by the Earth through the atmosphere, surface land, clouds etc.
Now, radiative balance is achieved when a planet's surface continuously warms up until it reaches its peak at which point the same amount of absorbed energy can then be radiated back to space. The relative amount of energy radiated back by a planet is dependent upon the size of the planet.
A colder planet relatively absorbs lower amount of radiation energy from space. In some time, as the planet heats up enough, the energy is radiated back to the space attaining thermal equilibrium.
Learn more about Stefan-Boltzmann law here:
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The total kinetic and potential energies
Answer:
The answer is
<h2>270 m</h2>
Explanation:
To find the distance when given the velocity and time we use the formula
<h3>distance = velocity × time</h3>
From the question
velocity of the ball = 18 m/s
time = 15 s
So the distance is
distance = 18 × 15
We have the final answer as
<h3>270 m</h3>
Hope this helps you
Answer:
3.2075*10^16
Explanation:
Q=P/V just search up a converter and youll get 30V and so you do 15/30 which is a half and a single coulomb is 6.415*10^16 so you half it. I belive this is correct if you dont belive me wait for someone else smarter to answer and compare.
Answer:
Explanation:
The ratio of pressure 2 to 1 us 5.48/1= 5.48 rounded off as 5.5.
Referring to table A.2 of modern compressible flow then 
Also
and making 
the subject of the formula then
Making reference to 
diagram then
