University Physics with Modern Physics (14th Edition)
14th Edition
ISBN: 9780321973610
Author: Hugh D. Young, Roger A. Freedman
Publisher: PEARSON
expand_more
expand_more
format_list_bulleted
Concept explainers
Videos
Textbook Question
Chapter 39, Problem 39.60P
An Ideal Blackbody. A large cavity that has a very small hole and is maintained at a temperature T is a good approximation to an ideal radiator or blackbody.
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solution
Students have asked these similar questions
A large cavity that has a very small hole and is maintained at a temperature T is a good approximation to an ideal radiator or blackbody. Radiation can pass into or out of the cavity only through the hole. The cavity is a perfect absorber, since any radiation incident on the hole becomes trapped inside the cavity. Such a cavity at 400°C has a hole with area 4.00 mm2. How long does it take for the cavity to radiate 100 J of energy through the hole?
The filament of a light bulb is cylindrical with length I = 20
mm and radius r = 0.05 mm. The filament is maintained
at a temperature T =
filament behaves approximately as a black body. What is
the total power radiated by the filament.
5000 K by an electric current. The
The eye of a stove top has a total area of 0.0628 m2 and gives off energy at a rate of 8720 W. If we assume the stove top eye to be a perfect blackbody, what would be the temperature of the eye in Kelvin?
Chapter 39 Solutions
University Physics with Modern Physics (14th Edition)
Ch. 39.2 - Prob. 39.2TYUCh. 39.3 - Prob. 39.3TYUCh. 39.4 - Prob. 39.4TYUCh. 39.5 - Prob. 39.5TYUCh. 39.6 - Prob. 39.6TYUCh. 39 - Prob. 39.1DQCh. 39 - Prob. 39.2DQCh. 39 - Prob. 39.3DQCh. 39 - When an electron beam goes through a very small...Ch. 39 - Prob. 39.5DQ
Ch. 39 - Prob. 39.6DQCh. 39 - Prob. 39.7DQCh. 39 - Prob. 39.8DQCh. 39 - Prob. 39.9DQCh. 39 - Prob. 39.10DQCh. 39 - Prob. 39.11DQCh. 39 - Prob. 39.12DQCh. 39 - Prob. 39.13DQCh. 39 - Prob. 39.14DQCh. 39 - Prob. 39.15DQCh. 39 - Prob. 39.16DQCh. 39 - Prob. 39.17DQCh. 39 - Prob. 39.18DQCh. 39 - Prob. 39.19DQCh. 39 - Prob. 39.20DQCh. 39 - Prob. 39.21DQCh. 39 - When you check the air pressure in a tire, a...Ch. 39 - Prob. 39.1ECh. 39 - Prob. 39.2ECh. 39 - Prob. 39.3ECh. 39 - Prob. 39.4ECh. 39 - Prob. 39.5ECh. 39 - Prob. 39.6ECh. 39 - Prob. 39.7ECh. 39 - Prob. 39.8ECh. 39 - Prob. 39.9ECh. 39 - Prob. 39.10ECh. 39 - Prob. 39.11ECh. 39 - Prob. 39.12ECh. 39 - Prob. 39.13ECh. 39 - Prob. 39.14ECh. 39 - Prob. 39.15ECh. 39 - Prob. 39.16ECh. 39 - Prob. 39.17ECh. 39 - Prob. 39.18ECh. 39 - Prob. 39.19ECh. 39 - Prob. 39.20ECh. 39 - Prob. 39.21ECh. 39 - Prob. 39.22ECh. 39 - Prob. 39.23ECh. 39 - Prob. 39.24ECh. 39 - Prob. 39.25ECh. 39 - Prob. 39.26ECh. 39 - Prob. 39.27ECh. 39 - Prob. 39.28ECh. 39 - Prob. 39.29ECh. 39 - Prob. 39.30ECh. 39 - Prob. 39.31ECh. 39 - Prob. 39.32ECh. 39 - Prob. 39.33ECh. 39 - Prob. 39.34ECh. 39 - Prob. 39.35ECh. 39 - Prob. 39.36ECh. 39 - Prob. 39.37ECh. 39 - Prob. 39.38ECh. 39 - Prob. 39.39ECh. 39 - Prob. 39.40ECh. 39 - Prob. 39.41ECh. 39 - Prob. 39.42ECh. 39 - Prob. 39.43ECh. 39 - Prob. 39.44ECh. 39 - Prob. 39.45ECh. 39 - Prob. 39.46ECh. 39 - Prob. 39.47ECh. 39 - Prob. 39.48ECh. 39 - Prob. 39.49ECh. 39 - Prob. 39.50PCh. 39 - Prob. 39.51PCh. 39 - Prob. 39.52PCh. 39 - Prob. 39.53PCh. 39 - Prob. 39.54PCh. 39 - Prob. 39.55PCh. 39 - Prob. 39.56PCh. 39 - Prob. 39.57PCh. 39 - Prob. 39.58PCh. 39 - Prob. 39.59PCh. 39 - An Ideal Blackbody. A large cavity that has a very...Ch. 39 - Prob. 39.61PCh. 39 - Prob. 39.62PCh. 39 - Prob. 39.63PCh. 39 - Prob. 39.64PCh. 39 - Prob. 39.65PCh. 39 - Prob. 39.66PCh. 39 - Prob. 39.67PCh. 39 - Prob. 39.68PCh. 39 - Prob. 39.69PCh. 39 - Prob. 39.70PCh. 39 - Prob. 39.71PCh. 39 - Prob. 39.72PCh. 39 - Prob. 39.73PCh. 39 - Prob. 39.74PCh. 39 - Prob. 39.75PCh. 39 - Prob. 39.76PCh. 39 - Prob. 39.77PCh. 39 - Prob. 39.78PCh. 39 - Prob. 39.79PCh. 39 - Prob. 39.80PCh. 39 - A particle with mass m moves in a potential U(x) =...Ch. 39 - Prob. 39.82PCh. 39 - Prob. 39.83PCh. 39 - DATA In the crystallography lab where you work,...Ch. 39 - Prob. 39.85PCh. 39 - Prob. 39.86CPCh. 39 - Prob. 39.87CPCh. 39 - Prob. 39.88PPCh. 39 - Prob. 39.89PPCh. 39 - Prob. 39.90PPCh. 39 - Prob. 39.91PP
Additional Science Textbook Solutions
Find more solutions based on key concepts
BIO Electric discharge by eels In several aquatic animals such as the South American electric eel electric orga...
College Physics
The equation P = V2/R indicates that the power dissipated in a resistor decreases if the resistance is increase...
Physics for Scientists and Engineers with Modern Physics
The position of a particle is given by r(t)=A(cost i +sint j ) . where is a constant. (a) Show that the parti...
University Physics Volume 1
The speed of the person sitting on the chair relative to the chair and relative to Earth.
Conceptual Physics (12th Edition)
21. Distinguish between constructive interference and destructive interference.
Conceptual Physical Science (6th Edition)
Choose the best answer to each of the following. Explain your reasoning. If Earth were twice as far as it actua...
The Cosmic Perspective Fundamentals (2nd Edition)
Knowledge Booster
Learn more about
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
- A: pherical body of 2.0 cm diameter is maintained at 500 °C. Assuming that it radiates as if it is a blackbody, at what rate is energy radiated from the sphere? O 35.2 W O 41 W O 52 W Not any of the choices listed 25.5 Warrow_forwardQuestion 8. The filament of a light bulb has a surface area 64 mm2. The filament can be considered as a black body at temperature 2500 K emitting radiation like a point source when viewed from far. At night the light bulb is observed from a distance of 100 m. Assume the pupil of the eyes of the observer to be circular with radius 3 mm. Then (Take Stefan-Boltzmann constant = 5.67 × 10−8 Wm−2K−4, Wien’s displacement constant = 2.90 × 10−3m-K, Planck’s constant = 6.63 × 10−34Js, speed of light in vacuum = 3.00 ×108 ms−1) a) power radiated by the filament is in the range 642 W to 645 W b) radiated power entering into one eye of the observer is in the range 3.15 × 10−8 W to 3.25 × 10−8 W c) the wavelength corresponding to the maximum intensity of light is 1160 nm d) taking the average wavelength of emitted radiation to be 1740 nm, the total number of photons entering per second into one eye of the observer is in the range 2.75 × 1011 to 2.85 × 1011arrow_forwardWe can use Stefan-Boltzmann Law, P = o AeT“, to produce a very rough estimation of temperature of the Earth. Follow the steps below to estimate the temperature of the Earth. At the radius of the Earth's orbit (1 astronomical unit away from the Sun), the thermal radiation from the Sun has an intensity of about S = 1370 W/m², known as the "solar constant." a. In terms of solar constant S and radius of the Earth R, what is the total solar power (Pn) incident on and absorbed by the Earth? Assume that Earth can be treated like a blackbody and will absorb all radiation incident on it. Hint for (a) Pin Give your answer in terms of S, R, and other numerical constants (spell out Greek characters, i.e. "pi" for T). the Earth rises, the power emitted by the Earth (Pout) increases. Give an b. As the temperature expression for power emitted by the Earth, in terms of its radius and other constants (see some of the constants used in Stefan-Boltzmann Law). Hint for (b) Pout Give your answer in terms…arrow_forward
- We can use Stefan-Boltzmann Law, P = o AeT“, to produce a very rough estimation of temperature of the Earth. Follow the steps below to estimate the temperature of the Earth. At the radius of the Earth's orbit (1 astronomical unit away from the Sun), the thermal radiation from the Sun has an intensity of about S = 1370 W/m², known as the "solar constant." a. In terms of solar constant S and radius of the Earth R, what is the total solar power (Pin) incident on and absorbed by the Earth? Assume that Earth can be treated like a blackbody and will absorb all radiation incident on it. Hint for (a) Pin Give your answer in terms of S, R, and other numerical constants (spell out Greek characters, i.e. "pi" for T). b. As the temperature of the Earth rises, the power emitted by the Earth (Pout) increases. Give an expression for power emitted by the Earth, in terms of its radius and other constants (see some of the constants used in Stefan-Boltzmann Law). Hint for (b) Pout Give your answer in…arrow_forwardA student is trying to decide what to wear.His bedroom is at 20°c.His skin Temperature is 35.0°c.The area of his exposed skin is 1.50 sq.mitres.People all over the world have skin that is dark in the infrared,with emessivity about 0.900.Find the net energy transfer from his body by radiation in 10.0 minutes.arrow_forwardAn incandescent lamp filament, with a surface area of 100mm^2, operates at a temperature of 2300 degrees Celsius. Assume that the filament acts like a blackbody(e = 1). (a) What is the rate of radiation from the filament? (b) If the walls of the room in which the lampoperates are at 27 degrees Celsius. What is the rate at which the filament absorbs radiation? (c) At what rate does electrical energy have to be supplied to the filament to keep its temperatureconstant? (Ignore conduction and convection losses from the filament.)arrow_forward
- Our sun is a standard sequence yellow dwarf star with a temperature of about 6000 K and a radius of about 7 x 10^8 m, emitting about 3.8 x 10^26 W. There are yellow giant stars with the same blackbody color (temperature) but with a radius 10 times larger than our sun (7 x 10^9 m). Estimate the power (emitted radiation) from one of these yellow giant stars.arrow_forwardThe Stefan-Boltzmann Law says that the light radiated from a perfect radiator ("blackbody") is proportional to the temperature raised to the fourth power: where σ is the Stefan-Boltzmann constrant (σ = 5.67 x 10-8 in MKS units) In equilibrium, F coming in equals F going out. At Mars' distance from the Sun, F coming in is 153 in MKS units. What is the blackbody temperature for Mars at a distance of 1.524 AU from the Sun?arrow_forwardThe radiation energy (intensity of the radiation) reaching Earth from the sun at the top of the atmosphere is 1.36×10^3??2⁄, which is called the solar constant. Assuming that Earth absorbs the total power coming from the Sun to the Earth and radiates with the emissivity of 0.8 (not ideal black body) at a uniform temperature around the Earth, what would the equilibrium temperature of Earth be?arrow_forward
- A large cavity that has a very small hole and is maintained at a temperature T is a good approximation to an ideal radiator or blackbody. Radiation can pass into or out of the cavity only through the hole. The cavity is a perfect absorber, since any radiation incident on the hole becomes trapped inside the cavity. Such a cavity at 400 •C has a hole with area 6.00 mm2. How long does it take for the cavity to radiate 300 J of energy through the hole?arrow_forwardThe energy reaching Earth from the Sun at the top of the atmosphere is 1.36 x10^3 W/m2, called the solar constant. Assuming that Earth radiates like a blackbody at uniform temperature, what do you conclude is the equilibrium temperature of Earth?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 1.61 m, a width of 37.5 cm and a length of 22.0 cm. Calculate the power emitted by the human body. What is the wavelength of the peak in the spectral distribution for this temperature? Fortunately our environment radiates too. The human body absorbs this radiation with an absorptance 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 23.5 °C? How much energy does our body lose in one second?arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
College PhysicsPhysicsISBN:9781305952300Author:Raymond A. Serway, Chris VuillePublisher:Cengage Learning
University Physics (14th Edition)PhysicsISBN:9780133969290Author:Hugh D. Young, Roger A. FreedmanPublisher:PEARSON
Introduction To Quantum MechanicsPhysicsISBN:9781107189638Author:Griffiths, David J., Schroeter, Darrell F.Publisher:Cambridge University Press
Physics for Scientists and EngineersPhysicsISBN:9781337553278Author:Raymond A. Serway, John W. JewettPublisher:Cengage Learning
Lecture- Tutorials for Introductory AstronomyPhysicsISBN:9780321820464Author:Edward E. Prather, Tim P. Slater, Jeff P. Adams, Gina BrissendenPublisher:Addison-Wesley
College Physics: A Strategic Approach (4th Editio...PhysicsISBN:9780134609034Author:Randall D. Knight (Professor Emeritus), Brian Jones, Stuart FieldPublisher:PEARSON
College Physics
Physics
ISBN:9781305952300
Author:Raymond A. Serway, Chris Vuille
Publisher:Cengage Learning
University Physics (14th Edition)
Physics
ISBN:9780133969290
Author:Hugh D. Young, Roger A. Freedman
Publisher:PEARSON
Introduction To Quantum Mechanics
Physics
ISBN:9781107189638
Author:Griffiths, David J., Schroeter, Darrell F.
Publisher:Cambridge University Press
Physics for Scientists and Engineers
Physics
ISBN:9781337553278
Author:Raymond A. Serway, John W. Jewett
Publisher:Cengage Learning
Lecture- Tutorials for Introductory Astronomy
Physics
ISBN:9780321820464
Author:Edward E. Prather, Tim P. Slater, Jeff P. Adams, Gina Brissenden
Publisher:Addison-Wesley
College Physics: A Strategic Approach (4th Editio...
Physics
ISBN:9780134609034
Author:Randall D. Knight (Professor Emeritus), Brian Jones, Stuart Field
Publisher:PEARSON
Heat Transfer: Crash Course Engineering #14; Author: CrashCourse;https://www.youtube.com/watch?v=YK7G6l_K6sA;License: Standard YouTube License, CC-BY