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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Answer:
A rotation occurs after every side out, which is when the receiving team gains the right to serve by winning a rally. ... The new serving team will rotate clockwise one spot. The purpose of this is to rotate all the players through the serving position. If you continue winning points, you stay in position.
Answer:
Ep = 117600 J
Explanation:
Data:
- Mass (m) = 600 kg
- Height (h) = 20 m
- Gravity (g) = 9.8 m/s²
- Potential Energy (Ep) = ?
Use formula:
Replace:
- Ep = 600 kg * 9.8 m/s² * 20 m
Multiply operations, and units:
What is the potential energy?
The potential energy is <u>117600 Joules.</u>
A. All natural radiation is at a level low enough to be safe
All machines are not 100% efficient because of <span>C. Friction</span>
