The surface of the Sun has a temperature of about 5800 K . The radius of the Sun is 6.96 ×10^8 m

Name: Problem 47, Chapter 20: Physics for Scientists and Engineers with Modern Physics
Uploaded: 2020-09-13T10:34:26-08:00
Duration: 2 min 1 s
Channel: Shahab Ullah
Description: The surface of the Sun has a temperature of about 5800 K . The radius of the Sun is 6.96 ×10^8 m . Calculate the total energy radiated by the Sun each second. Assume that the emissivity of the Sun is 0.965 .

step 1 In this problem we are given the surface temperature of sun is equal to 5 ,800 Kelvin and the ra

Question

The surface of the Sun has a temperature of about 5800 $\mathrm{K}$ . The radius of the Sun is $6.96 \times 10^{8} \mathrm{m} .$ Calculate the total energy radiated by the Sun each second. Assume that the emissivity of the Sun is $0.965 .$

   The surface of the Sun has a temperature of about 5800 $\mathrm{K}$ . The radius of the Sun is $6.96 \times 10^{8} \mathrm{m} .$ Calculate the total energy radiated by the Sun each second. Assume that the emissivity of the Sun is $0.965 .$

Physics for Scientists and Engineers with Modern Physics

Paul Tipler, Gene… 6th Edition

Chapter 20, Problem 47

Instant Answer

Solved by Expert Shahab Ullah

09/13/2020

Step 1

96 \times 10^{8} \, \mathrm{m}$, and the emissivity of the Sun $e = 0.965$. We are also given the Stefan-Boltzmann constant $\sigma = 5.67 \times 10^{-8} \, \mathrm{W} \, \mathrm{m}^{-2} \, \mathrm{K}^{-4}$. Show more…

Show all steps

Thanks for your feedback!

The surface of the Sun has a temperature of about 5800 $\mathrm{K}$ . The radius of the Sun is $6.96 \times 10^{8} \mathrm{m} .$ Calculate the total energy radiated by the Sun each second. Assume that the emissivity of the Sun is $0.965 .$

Play audio

Feedback

Labs

Want to see this concept in action?

NEW

Explore this concept interactively to see how it behaves as you change inputs.

View Labs

Key Concepts

Emissivity

Emissivity is a dimensionless factor that indicates how efficiently a real surface emits thermal radiation compared to a perfect blackbody. It ranges between 0 and 1; a value less than 1 means that the object emits less radiation than an ideal blackbody at the same temperature.

Surface Area of a Sphere

The surface area of a sphere is calculated using the formula 4?R², where R is the radius. In astrophysics, this concept is used to scale the local energy flux emitted per unit area (from the Stefan-Boltzmann law) over the entire surface of a spherical body, such as a star, to determine its total energy output or luminosity.

Stefan-Boltzmann Law

This law states that a blackbody radiates energy at a rate proportional to the fourth power of its absolute temperature, encapsulated in the formula E = ?T?, where ? is the Stefan-Boltzmann constant. It is a fundamental result in thermodynamics and astrophysics for calculating thermal radiation emitted by objects.

Please give Ace some feedback