Modern Physics for Scientists and Engineers
4th Edition
ISBN: 9781133103721
Author: Stephen T. Thornton, Andrew Rex
Publisher: Cengage Learning
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Chapter 3, Problem 26P
(a)
To determine
The power
(b)
To determine
The power radiated by the person’s body at the normal temperature.
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Chapter 3 Solutions
Modern Physics for Scientists and Engineers
Ch. 3 - Prob. 1QCh. 3 - Prob. 2QCh. 3 - Prob. 3QCh. 3 - Prob. 4QCh. 3 - Prob. 5QCh. 3 - Prob. 6QCh. 3 - Prob. 7QCh. 3 - Prob. 8QCh. 3 - Prob. 9QCh. 3 - In the experiment of Example 3.2, how could you...
Ch. 3 - Prob. 11QCh. 3 - Prob. 12QCh. 3 - Prob. 13QCh. 3 - Prob. 14QCh. 3 - Prob. 15QCh. 3 - Prob. 16QCh. 3 - Prob. 17QCh. 3 - Prob. 18QCh. 3 - Prob. 19QCh. 3 - Prob. 20QCh. 3 - Prob. 21QCh. 3 - Prob. 22QCh. 3 - Prob. 23QCh. 3 - Prob. 24QCh. 3 - Prob. 25QCh. 3 - Prob. 26QCh. 3 - Prob. 1PCh. 3 - Prob. 2PCh. 3 - Across what potential difference does an electron...Ch. 3 - Prob. 4PCh. 3 - Prob. 5PCh. 3 - Prob. 6PCh. 3 - Prob. 7PCh. 3 - Prob. 8PCh. 3 - Prob. 9PCh. 3 - Prob. 10PCh. 3 - Prob. 11PCh. 3 - Prob. 12PCh. 3 - Prob. 13PCh. 3 - Prob. 14PCh. 3 - Prob. 15PCh. 3 - Prob. 16PCh. 3 - Calculate max for blackbody radiation for (a)...Ch. 3 - Prob. 18PCh. 3 - Prob. 19PCh. 3 - Prob. 20PCh. 3 - White dwarf stars have been observed with a...Ch. 3 - Prob. 22PCh. 3 - Prob. 23PCh. 3 - Prob. 24PCh. 3 - Prob. 25PCh. 3 - Prob. 26PCh. 3 - Prob. 27PCh. 3 - Prob. 32PCh. 3 - Prob. 33PCh. 3 - Prob. 34PCh. 3 - Prob. 35PCh. 3 - Prob. 36PCh. 3 - Prob. 37PCh. 3 - Prob. 38PCh. 3 - Prob. 39PCh. 3 - Prob. 40PCh. 3 - Prob. 41PCh. 3 - Prob. 42PCh. 3 - Prob. 43PCh. 3 - Prob. 44PCh. 3 - Prob. 45PCh. 3 - Prob. 46PCh. 3 - Prob. 47PCh. 3 - Prob. 48PCh. 3 - Prob. 49PCh. 3 - Prob. 50PCh. 3 - Prob. 52PCh. 3 - Prob. 53PCh. 3 - Prob. 54PCh. 3 - Prob. 55PCh. 3 - Prob. 56PCh. 3 - Prob. 57PCh. 3 - Prob. 58PCh. 3 - Prob. 59PCh. 3 - Prob. 60PCh. 3 - Prob. 61PCh. 3 - Prob. 62PCh. 3 - Prob. 63PCh. 3 - Prob. 64PCh. 3 - Prob. 65PCh. 3 - Prob. 66PCh. 3 - Prob. 67PCh. 3 - Prob. 68PCh. 3 - The Fermi Gamma-ray Space Telescope, launched in...Ch. 3 - Prob. 70P
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- The 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_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_forwardA 100 W incandescent light bulb has a cylindrical tungsten filament 30.0 cm long, 0.40 mm in diameter, and with an emissivity of 0.26. (a) What is the temperature of the filament? (b) For what wave- length does the spectral emittance of the bulb peak? (c) Incandescent light bulbs are not very efficient sources of visible light. Explain why this is so.arrow_forward
- Estimate the peak wavelength of light emitted from the pupil of the human eye (which approximates a blackbody) assuming normal body temperature.arrow_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 radius of our Sun is 6.96 x 10° m, and its total power output is 3.85 x 1020 W. (a) Assuming the Sun's surface emits as a black- body, calculate its surface temperature. (b) Using the result of part (a), find Amax for the Sun.arrow_forwardUsing Stefan's law to calculate the total power radiated per square meter by a filament at 1827 °C having an absorption factor of 0.54.arrow_forwardAt what wavelength will the human body radiate the maximum radiation? (a) Estimate the total power radiated by a person of medium build (assume an area given by a cylinder of 175-cm height and 13-cm radius). (b) Using your answer to (a), compare the energy radiated by a person in one day with the energy intake of a 2000-kcal diet.arrow_forward
- An incandescent lightbulb contains a tung-sten filament that reaches a temperature of about 3020 K, roughly half the surface temperature of the Sun. (a) Treating the filament as a blackbody, determine the frequency for which its radiation is a maximum. (b) Do you expect the lightbulb to radiate more energy in the visible or in the infrared part of the spectrum? Explain.arrow_forwardThe temperature of an electric heating element is 150°C. At what wavelength does the radiation emitted from the heating element reach its peak? Model the tungsten filament of a lightbulb as a black body at temperature 2 900 K. (a) Determine the wave- length of light it emits most strongly. (b) Explain why the answer to part (a) suggests that more energy from the lightbulb goes into infrared radiation than into vis- ible light.arrow_forwardThe 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.arrow_forward
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