On a given day, solar energy strikes the top of the Earth's atmosphere at 346 W·m−2....
On a given day, solar energy strikes the top of the Earth's
atmosphere at 346 W·m−2. About 30. percent of this
energy is reflected directly back into space. The Earth-atmosphere
system absorbs the remaining energy and re-radiates it into space
as black-body radiation at 5.672 ✕
10−8(T/K)4 W·m−2, where
T is the temperature.
a) Assuming that the arrangement has come to equilibrium, what is
the average black-body temperature (in K) of the Earth?
b) Calculate the wavelength (in m) at which the black-body radiation from the Earth is at a maximum. (Hint: Recall Wien's law λmaxT =
| hc |
|
4.965k For a) I got 180.77. a) I got 5.53e-3 not sure what I'm doing wrong. Please show work, Thanks |
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On a given day, solar energy strikes the top of the Earth's atmosphere at 346 W·m−2....
2. (5 points) Solar radiation strikes Earth's atmosphere each day. These collisions knock electrons off of...
2. (5 points) Solar radiation strikes Earth's atmosphere each day. These collisions knock electrons off of atoms and create very many ions. Rain carries the electrons to the ground so that, to a good approximation, Earth's surface can be thought of as a uniform shell of negative charge-Q and the atmosphere can be thought of as a concentric shell of positive charge +Q. What is the magnitude of the resulting electric field (due to this arrangement of charges) that an...
About 71 percent of the total incoming solar energy is absorbed by the earth system, the...
About 71 percent of the total incoming solar energy is absorbed by the earth system, the 29% is reflected back to space by clouds, about 23 percent of incoming solar energy is absorbed in the atmosphere by water vapor. The rest (48%) passes through the atmosphere and is absorbed by the surface. If the sun’s diameter is 1,392,000 km, and it emits energy as if it were a black body at 5777 K. Determine the solar heat transfer and heat...
On a clear day, the total intensity of solar radiation incident at the Earth's surface is...
On a clear day, the total intensity of solar radiation incident at the Earth's surface is approximately 1000W/m2 Part a Assume our atmosphere absorbs 23% of the incoming solar radiation, and that the distance from the Earth to the Sun is 1.5 x 1011m. From this information, what do you expect is the total power output of the sun? [IMPORTANT: to express a number like 2 x 1021, type 2e21] Enter answer here O of 4 attempts used CHECK ANSWER...
1. The solar energy spectral density is shown in the right figure. By assuming that the...
1. The solar energy spectral density is shown in the right figure. By assuming that the sun is a blackbody, use the Planck's distribution function to fit the extraterrestrial solar energy spectral density. Extraterrestrial (a) Determine the most possible surface temperature T of sun by fitting the Planck's distribution to the extraterrestrial solar energy spectral density. You can choose a few temperatures to see which temperature can best fit the peak (at Amsx) and the entire profile of the extraterrestrial...
u(λ,T)=4E(λ,T)/c 2. Use the energy density expression above and the Stefan-Boltzmann expression, u(T) 014 with σ=...
u(λ,T)=4E(λ,T)/c
2. Use the energy density expression above and the Stefan-Boltzmann expression, u(T) 014 with σ= 7.56x 10.15 erg/cmK4, to obtain a formula for the total rate of radiation per unit area of a black body. Assume that the sun radiates as a black body. You are given the radius of the sun R -7x101° cm, the average distance of the sun to the earth d Lx10 c, nthe solar consdant, the aount of enexgy : carth when the sun...
How much power (power is the energy per second) is radiated by the person
Radiation of Energy The rate of heat transfer by emitted radiation is determined by the Stefan-Boltzmann law of radiation: = aeAT4 where o 5.67x10-8 J/s - m2 K is the Stefan-Boltzmann constant, A is the surface area of the object, and T is its absolute temperature in kelvin. The symbol e stands for the emissivity of the object, which is a measure of how well it radiates An ideal jet-black (or black body) radiator has e 1,whereas a perfect reflector has...
I can see here that for question B Stefan–Boltzmann law was used. However, the energy per unit area is being divided per 4. why? The ratio distance of Mars from the Sun 1.5 6. distance of Earth from...
I can see here that for question B Stefan–Boltzmann law was
used. However, the energy per unit area is being divided per 4.
why?
The ratio distance of Mars from the Sun 1.5 6. distance of Earth from the Sun (a) Show that the intensity of solar radiation at the orbit of Mars is about 600 W m2 (b) Determine, in K, the mean surface temperature of Mars. Assume that Mars acts as a black body. 121 (c) The atmosphere...
Answer all parts except the ones refering to lecture slides. Temperatures on planets. To a good...
Answer all parts except the ones refering to lecture slides.
Temperatures on planets. To a good approximation, stars and planets emit their energy like a black body, which means the energy flux (energy per unit area and per unit time) at the solar surface (radius R_s = 7 times 10^8 m) is given by F = sigma_SBT^4, where sigma_SB = 5.67 times 10^8 W m^-2 K^-41 is the Stefan-Boltzmann constant. [Remember, energy per unit time is power and it- is...
Problem 24.1: please help!! Solar Thermal Energy 462 onsider a solur thermal elecinic plant built using a system of 2D...
Problem 24.1: please help!!
Solar Thermal Energy 462 onsider a solur thermal elecinic plant built using a system of 2D concentrators that reflect sunight to a system of pipes carrying molten salt with concentration C # 200. Example 24.5 2D Concentrator Efficiency Optimization Wher is the optimal efficiency poxsibie (essaming an onbient temperoture of 300 K and incident sunight u 1000 W/r)? Solving eq (24.23) un encany gives 818 K At this temperature. Cartot efficiency is approximately 63% and about...
Please use the formulate sheet and show all steps to make sure the question is worth...
Please use the formulate sheet and show all steps to make sure
the question is worth any points
a) The initial ratio of deuterium (D) to hydrogen (H) in a planet's atmosphere was 175000; however, the present ratio is 1/1500 and the initial and final abundances of D are 5 x 10° atoms per m3 and 9 x 106 atoms per m2, respectively. What fraction of deuterium has been lost, and what fraction of hydrogen has been lost in this...
2. (5 points) Solar radiation strikes Earth's atmosphere each day. These collisions knock electrons off of atoms and create very many ions. Rain carries the electrons to the ground so that, to a good approximation, Earth's surface can be thought of as a uniform shell of negative charge-Q and the atmosphere can be thought of as a concentric shell of positive charge +Q. What is the magnitude of the resulting electric field (due to this arrangement of charges) that an...
On a clear day, the total intensity of solar radiation incident at the Earth's surface is approximately 1000W/m2 Part a Assume our atmosphere absorbs 23% of the incoming solar radiation, and that the distance from the Earth to the Sun is 1.5 x 1011m. From this information, what do you expect is the total power output of the sun? [IMPORTANT: to express a number like 2 x 1021, type 2e21] Enter answer here O of 4 attempts used CHECK ANSWER...
1. The solar energy spectral density is shown in the right figure. By assuming that the sun is a blackbody, use the Planck's distribution function to fit the extraterrestrial solar energy spectral density. Extraterrestrial (a) Determine the most possible surface temperature T of sun by fitting the Planck's distribution to the extraterrestrial solar energy spectral density. You can choose a few temperatures to see which temperature can best fit the peak (at Amsx) and the entire profile of the extraterrestrial...
u(λ,T)=4E(λ,T)/c
2. Use the energy density expression above and the Stefan-Boltzmann expression, u(T) 014 with σ= 7.56x 10.15 erg/cmK4, to obtain a formula for the total rate of radiation per unit area of a black body. Assume that the sun radiates as a black body. You are given the radius of the sun R -7x101° cm, the average distance of the sun to the earth d Lx10 c, nthe solar consdant, the aount of enexgy : carth when the sun...
Radiation of Energy The rate of heat transfer by emitted radiation is determined by the Stefan-Boltzmann law of radiation: = aeAT4 where o 5.67x10-8 J/s - m2 K is the Stefan-Boltzmann constant, A is the surface area of the object, and T is its absolute temperature in kelvin. The symbol e stands for the emissivity of the object, which is a measure of how well it radiates An ideal jet-black (or black body) radiator has e 1,whereas a perfect reflector has...
I can see here that for question B Stefan–Boltzmann law was
used. However, the energy per unit area is being divided per 4.
why?
The ratio distance of Mars from the Sun 1.5 6. distance of Earth from the Sun (a) Show that the intensity of solar radiation at the orbit of Mars is about 600 W m2 (b) Determine, in K, the mean surface temperature of Mars. Assume that Mars acts as a black body. 121 (c) The atmosphere...
Answer all parts except the ones refering to lecture slides.
Temperatures on planets. To a good approximation, stars and planets emit their energy like a black body, which means the energy flux (energy per unit area and per unit time) at the solar surface (radius R_s = 7 times 10^8 m) is given by F = sigma_SBT^4, where sigma_SB = 5.67 times 10^8 W m^-2 K^-41 is the Stefan-Boltzmann constant. [Remember, energy per unit time is power and it- is...
Problem 24.1: please help!!
Solar Thermal Energy 462 onsider a solur thermal elecinic plant built using a system of 2D concentrators that reflect sunight to a system of pipes carrying molten salt with concentration C # 200. Example 24.5 2D Concentrator Efficiency Optimization Wher is the optimal efficiency poxsibie (essaming an onbient temperoture of 300 K and incident sunight u 1000 W/r)? Solving eq (24.23) un encany gives 818 K At this temperature. Cartot efficiency is approximately 63% and about...
Please use the formulate sheet and show all steps to make sure
the question is worth any points
a) The initial ratio of deuterium (D) to hydrogen (H) in a planet's atmosphere was 175000; however, the present ratio is 1/1500 and the initial and final abundances of D are 5 x 10° atoms per m3 and 9 x 106 atoms per m2, respectively. What fraction of deuterium has been lost, and what fraction of hydrogen has been lost in this...
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