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:
ξ = 0.00845020162 V or 8.4 mV
Explanation:
Magnetic flux measures the total magnetic field that passes through a known area. Magnetic flux describe the effect of magnetic field in a given area. Mathematically,
magnetic flux (Ф) = BA cos ∅
where
A = test area
B = magnetic field
before the flip
Ф = Bπr²N
N = number of turn
magnitude of induced emf = N |ΔФ/Δt|
ξ = 2Nπr²B/dt
ξ = 2 × 22 × π × (1.02/2)² × 0.000047/0.2
ξ = 44 × π × 0.51² × 0.000047/0.2
ξ = 44 × π × 0.2601 × 0.000047/0.2
ξ = 0.0005378868 × 3.142/0.2
ξ = 0.00169004032/0.2
ξ = 0.00845020162 V or 8.4 mV
