Radiation, Heat Transfer & the Stefan-Boltzmann Law

Lesson Transcript
Instructor: David Wood

David has taught Honors Physics, AP Physics, IB Physics and general science courses. He has a Masters in Education, and a Bachelors in Physics.

Radiation is a form of heat transfer that can be calculated using the Stefan-Boltzmann Law. Learn what radiation is, explore the vacuum flask example of radiation, then learn to explain the Stefan-Boltzmann law before applying it to a calculation example. Updated: 10/28/2021

What Is Radiation?

Ah, radiation! Run! That seems to be what people think of when you use the word radiation. But radiation has a few different meanings in physics. There is the dangerous radioactive type of radiation, made of alpha particles, beta particles and gamma rays - the kind of radiation that comic books tell us will turn you into the Hulk or some other equally cool superhero.

But the Sun also sends us radiation. The other, more general meaning of radiation is just a type of electromagnetic wave. Light is radiation, infrared is radiation, gamma rays are, too, it's true - but there's nothing inherently dangerous about radiation.

But in this lesson, we're talking about radiation as a type of heat transfer - the other two types of heat transfer being conduction and convection. Hot objects give off infrared radiation, which is just another part of the electromagnetic spectrum. But that infrared radiation also transfers heat away from that object. That's why it's hot when you stand next to a campfire. By the way, if you put your hand above a campfire, it's even hotter because then you not only have heating by radiation, but also by convection - another type of heat transfer.

So radiation is a type of heat transfer that travels through electromagnetic waves. Because of this, radiation doesn't need a medium (or material), and it can therefore go through a vacuum. This is how the heat of the Sun gets to us on Earth.

An error occurred trying to load this video.

Try refreshing the page, or contact customer support.

Coming up next: Thermal Expansion: Importance & Examples

You're on a roll. Keep up the good work!

Take Quiz Watch Next Lesson
Your next lesson will play in 10 seconds
  • 0:00 What is Radiation?
  • 1:24 Vacuum Flask
  • 1:58 The Stefan-Boltzmann Law
  • 2:54 Calculation Example
  • 3:52 Lesson Summary
Save Save Save

Want to watch this again later?

Log in or sign up to add this lesson to a Custom Course.

Log in or Sign up

Speed Speed

Example of Radiation: Vacuum Flask

So we've already talked about campfires and the heat energy from the Sun. But there are many examples of radiation in the real world.

A vacuum flask, or thermos flask, uses our understanding of radiation (and heat transfer in general) to keep your soup warm. We all know that light bounces off mirrors, but all electromagnetic waves tend to bounce off reflective surfaces. So the mirrored surface of a vacuum flask does a great job of stopping heat loss by radiation. A vacuum flask also stops conduction by having a vacuum layer - conduction needs a material to travel through and convection by having an insulating lid.

The Stefan-Boltzmann Law

The Stefan-Boltzmann Law gives us a way to put numbers to this concept of radiation. It helps us calculate the heat transferred by radiation per second, measured in joules per second, or watts. The Stefan-Boltzmann Law tells us that this is equal to the Stefan-Boltzmann constant sigma, which is always the same number, multiplied by the emissivity of the object (e), which is a number that represents how well an object radiates heat, multiplied by the surface area of the object (A) measured in meters squared, multiplied by the temperature of the object (T) to the power 4, where T is measured in Kelvin.

Stefan-Boltzmann Law
stefan boltzmann equation

A few things to note about this equation. The Stefan-Boltzmann constant is always 5.67 * 10^-8. The emissivity of an object is a number between zero and one. A perfect radiator of energy has an emissivity of one, and a perfect reflector has an emissivity of zero. Stars like the Sun have an emissivity extremely close to one.

To unlock this lesson you must be a Study.com Member.
Create your account

Register to view this lesson

Are you a student or a teacher?

Unlock Your Education

See for yourself why 30 million people use Study.com

Become a Study.com member and start learning now.
Become a Member  Back
What teachers are saying about Study.com
Try it now
Create an account to start this course today
Used by over 30 million students worldwide
Create an account