COLLEGE PHYSICS
2nd Edition
ISBN: 9781464196393
Author: Freedman
Publisher: MAC HIGHER
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Chapter 26, Problem 47QAP
To determine
The corresponding temperature of the Sun's outer layer
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The wavelength of maximum intensity of the sun’s radiation is observed to be near 500 nm. Assume the sun to be a blackbody and calculate (a) the sun’s surface temperature, (b) the power per unit area R(T) emitted from the sun’s surface, and (c) the energy received by the Earth each day from the sun’s radiation.
Problem-1:
An asteroid is hurtling toward earth at 150,000“. The temperature of the asteroid is about 100 K, meaning that its peak emission
is 2 = 29 µm. The speed of light is c =
3E[8].
a) What is the wavelength of light that we receive from the asteroid? (Answer: 2.89855E[-05] m)
>
In this problem you will consider the balance of thermal energy
radiated and absorbed by a person.
Assume that the person is wearing only a skimpy bathing suit of
negligible area. As a rough approximation, the area of a human
body may be considered to be that of the sides of a cylinder of
length L = 2.0 m and circumference C = 0.8 m.
For the Stefan-Boltzmann constant use
o= 5.67 x 10-8 W/m²/K4
Part C
Now calculate Por, the thermal power absorbed by the person from the thermal radiation field in the room, which is assumed to be at Troom = 20°C. If
you do not understand the role played by the emissivities of room and person, be sure to open the hint on that topic.
Express the thermal power numerically, giving your answer to the nearest 10 W.
View Available Hint(s)
Por=
Submit
Part D
[-] ΑΣΦ.
Pnet =
17] ΑΣΦ
Find Paet, the net power radiated by the person when in a room with temperature Troom= 20°C.
Express the net radiated power numerically, to the nearest 10 W.
▸ View Available Hint(s)…
Chapter 26 Solutions
COLLEGE PHYSICS
Ch. 26 - Prob. 1QAPCh. 26 - Prob. 2QAPCh. 26 - Prob. 3QAPCh. 26 - Prob. 4QAPCh. 26 - Prob. 5QAPCh. 26 - Prob. 6QAPCh. 26 - Prob. 7QAPCh. 26 - Prob. 8QAPCh. 26 - Prob. 9QAPCh. 26 - Prob. 10QAP
Ch. 26 - Prob. 11QAPCh. 26 - Prob. 12QAPCh. 26 - Prob. 13QAPCh. 26 - Prob. 14QAPCh. 26 - Prob. 15QAPCh. 26 - Prob. 16QAPCh. 26 - Prob. 17QAPCh. 26 - Prob. 18QAPCh. 26 - Prob. 19QAPCh. 26 - Prob. 20QAPCh. 26 - Prob. 21QAPCh. 26 - Prob. 22QAPCh. 26 - Prob. 23QAPCh. 26 - Prob. 24QAPCh. 26 - Prob. 25QAPCh. 26 - Prob. 26QAPCh. 26 - Prob. 27QAPCh. 26 - Prob. 28QAPCh. 26 - Prob. 29QAPCh. 26 - Prob. 30QAPCh. 26 - Prob. 31QAPCh. 26 - Prob. 32QAPCh. 26 - Prob. 33QAPCh. 26 - Prob. 34QAPCh. 26 - Prob. 35QAPCh. 26 - Prob. 36QAPCh. 26 - Prob. 37QAPCh. 26 - Prob. 38QAPCh. 26 - Prob. 39QAPCh. 26 - Prob. 40QAPCh. 26 - Prob. 41QAPCh. 26 - Prob. 42QAPCh. 26 - Prob. 43QAPCh. 26 - Prob. 44QAPCh. 26 - Prob. 45QAPCh. 26 - Prob. 46QAPCh. 26 - Prob. 47QAPCh. 26 - Prob. 48QAPCh. 26 - Prob. 49QAPCh. 26 - Prob. 50QAPCh. 26 - Prob. 51QAPCh. 26 - Prob. 52QAPCh. 26 - Prob. 53QAPCh. 26 - Prob. 54QAPCh. 26 - Prob. 55QAPCh. 26 - Prob. 56QAPCh. 26 - Prob. 57QAPCh. 26 - Prob. 58QAPCh. 26 - Prob. 59QAPCh. 26 - Prob. 60QAPCh. 26 - Prob. 61QAPCh. 26 - Prob. 62QAPCh. 26 - Prob. 63QAPCh. 26 - Prob. 64QAPCh. 26 - Prob. 65QAPCh. 26 - Prob. 66QAPCh. 26 - Prob. 67QAPCh. 26 - Prob. 68QAPCh. 26 - Prob. 69QAPCh. 26 - Prob. 70QAPCh. 26 - Prob. 71QAPCh. 26 - Prob. 72QAPCh. 26 - Prob. 73QAPCh. 26 - Prob. 74QAPCh. 26 - Prob. 75QAPCh. 26 - Prob. 76QAPCh. 26 - Prob. 77QAPCh. 26 - Prob. 78QAPCh. 26 - Prob. 79QAPCh. 26 - Prob. 80QAPCh. 26 - Prob. 81QAPCh. 26 - Prob. 82QAPCh. 26 - Prob. 83QAPCh. 26 - Prob. 84QAPCh. 26 - Prob. 85QAPCh. 26 - Prob. 86QAPCh. 26 - Prob. 87QAPCh. 26 - Prob. 88QAPCh. 26 - Prob. 89QAPCh. 26 - Prob. 90QAPCh. 26 - Prob. 91QAPCh. 26 - Prob. 92QAPCh. 26 - Prob. 93QAPCh. 26 - Prob. 94QAPCh. 26 - Prob. 95QAPCh. 26 - Prob. 96QAPCh. 26 - Prob. 97QAPCh. 26 - Prob. 98QAPCh. 26 - Prob. 99QAPCh. 26 - Prob. 100QAPCh. 26 - Prob. 101QAPCh. 26 - Prob. 102QAPCh. 26 - Prob. 103QAPCh. 26 - Prob. 104QAP
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Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Estimate the total energy loss by radiation if a person’s head is uncovered for 13.3 min on a very cold, −15.0°C day, assuming he is bald, his skin temperature is 35.0°C, and that skin has an emissivity (in the infrared) of 97.0%. Assume that the man’s head is spherical, with a radius of 10.0 cm. The Stefan–Boltzmann constant is 5.670 × 10−8 W/ (m2·K4).arrow_forwardThe wavelength at which the Sun emits its most intense light is about 550 nm. (The Sun's data can be found on the inside back cover of the book; use Stefan's Law to calculate the power.) a) Assuming the Sun radiates as a perfect blackbody, estimate its surface temperature. b) Assuming the Sun radiates as a perfect blackbody, estimate its total emitted power.arrow_forwardThe maximum intensity of radiation emitted by a star occurs at a surface temperature of 4.3 x 104 K. a) Calculate the wavelength of the emitted radiation when the intensity is maximum. b) Calculate the ratio of the intensity radiated at a wavelength of 60.0 nm to the maximum intensity. Assume that the star radiates like an ideal blackbody.arrow_forward
- A small satellite is in orbit around the Earth at a height of 1500 km above the surface. It has a mass of 100 kg, a diameter of 1 m, an absorptivity of 0.8 for IR radiation and 0.4 for visible radiation. a) What solid angle does the Earth subtend when viewed from the satellite? b) Calculate the radiative equilibrium temperature of the satellite when it is in the shadow of the Earth. c) What is the radiative equilibrium temperature of the satellite at the moment when it passes completely out of the shadow of the Earth? (Note that at this time the Earth is still completely dark when viewed from the satellite.)arrow_forwardDaylight and incandescent light may be approximated as a blackbody at the effective surface temperatures of 5800 K and 2800 K, respectively. Determine the wavelength at maximum emission of radiation for each of the lighting sources.arrow_forwardThe radius of our Sun is 6.96 x 108 m, and its total power output is 3.85 x 1026 W. Assuming the Sun's surface emits as a black body, calculate its surface temperature.arrow_forward
- The emissivity of the human skin is 97.0 percent. Use 35.0 °C for the skin temperature and approximate the human body by a rectangular block with a height of 1.66 m, a width of 31.0 cm and a length of 21.5 cm. Calculate the power emitted by the human body. Submit Answer Tries 0/20 What is the wavelength of the peak in the spectral distribution for this temperature? Submit Answer Tries 0/20 Fortunately our environment radiates too. The human body absorbs this radiation with an absorbance of 97.0 percent, so we don't lose our internal energy so quickly. How much power do we absorb when we are in a room where the temperature is 24.0 °C? Submit Answer Tries 0/20 How much energy does our body lose in one second? Submit Answer Tries 0/20arrow_forwardThe emissivity of the human skin is 97.0 percent. Use 35.0 °C for the skin temperature and approximate the human body by a rectangular block with a height of 1.98 m, a width of 35.5 cm and a length of 26.5 cm. Calculate the power emitted by the human body. 1.311x10³ W You are correct. Your receipt no. is 157-4629 Previous Tries What is the wavelength of the peak in the spectral distribution for this temperature? 8.56x10^-5m Hint: Use Wien's displacement law. Submit Answer Incorrect. Tries 3/12 Previous Tries Fortunately our environment radiates too. The human body absorbs this radiation with an absorbance of 97.0 percent, so we don't lose our internal energy so quickly. How much power do we absorb when we are in a room where the temperature is 20.5 °C? 625.36W Hint: Use the Stefan-Boltzmann law again. Submit Answer Incorrect. Tries 1/12 Previous Tries How much energy does our body lose in one second? Submit Answer Tries 0/12arrow_forwardQuestion A7 The intensity of the emitted radiation by a star is at a maximum at a wavelength of 78.9 nm. a) Calculate the surface temperature of the star. b) Calculate the ratio of the intensity radiated at 65.0 nm to the maximum intensity. Assume that the star radiates like an ideal blackbody.arrow_forward
- The wavelength of maximum solar emission is observed to be approximately 0.475 μm. What is the surface temperature of the sun (assumed as blackbody)?arrow_forward• The temperature at which the R.M.S. Velocity of hydrogen is four times of its value at NTP, isarrow_forwardWhat is the surface temperature of Betelgeuse, a red giant star in the constellation of Orion, which radiates with a peak wavelength of about 970 nm? (b) Rigel, a bluish - white star in Orion, radiates with a peak wavelength of 145 nm. Find the temperature of Rigel’s surface.arrow_forward
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