C++ for Engineers and Scientists
C++ for Engineers and Scientists
4th Edition
ISBN: 9781133187844
Author: Bronson, Gary J.
Publisher: Course Technology Ptr
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Chapter 1.2, Problem 7E

(a)

Program Plan Intro

To determine the resulting unit of radiated energy E by the given formula E=σ×T4 .

(b)

Program Plan Intro

To determine the energy radiated from the sun’s surface, it is given that the sun’s average temperature is approximately 6000oK.

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(Heat transfer) The energy radiated from the surface of the sun or a planet in the solar system can be calculated by using Stefan-Boltzmann's Law: E = o x T4 E is the energy radiated. o is Stefan-Boltzmann's constant (5.6697 x 10-8 watts/m2K4). Tis the surface temperature in degrees Kelvin (°K = °C + 273). a. Determine the units of E by calculating the units resulting from the right side of the formula. b. Determine the energy radiated from the sun's surface, given that the sun's average temperature is approximately 6000°K.

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