Understanding the Stefan-Boltzmann Law (when the surroundings are hotter)

In summary: Radiation will be the dominant mode of heat transfer in a vacuum or space.In summary, the Stefan-Boltzmann Law is formulated as ##H = A\sigma T^4## and represents the energy emitted per unit time. Emissivity is represented by ##e## and varies from 0 to 1 for real materials, while the Stefan-Boltzmann constant is represented by ##\sigma##. Newton's Law of Cooling is a special case of the Stefan-Boltzmann Law and is used when the temperature difference is small. Conduction is the time rate of heat flow for a given temperature difference and can be calculated using the formula ##H = kA \frac {T_c - T_d}{L}##
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JC2000
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1.My book tells me that given ##T_{surroundings}##, and ##T## of the object radiating heat, the law is expressed as ##H = \sigma A (T^4 - T^4_{surroundings})##.

2. Relating Newton's Law of Cooling, Conduction, and Stefan-Boltzmann Law

3. Is emissivity the same as Stefan's constant or is it ## e * \sigma## where ##e## varies, depending on the material?
1.If so what would the law mean if ##T_{surroundings}>T##?

2. Stefan-Boltzmann Law is formulated as ##H = A\sigma T^4## where ##H## is the energy emitted per unit time, ##A## is the area of the object, ##T## is the absolute temperature of the object and (3.) I am unclear about whether ##\sigma## represents emissivity or ##e*\sigma## represents Stefan's constant.

My book also defines Conduction (as the time rate of heat flow for a given temperature difference), as ##H = kA \frac {T_c - T_d}{L}## where ##H## is the rate of flow of heat (heat current), ##A## is the area of cross-section and ##L## is the length between the two points being considered, ##T_c - T_d## the temperature difference between the points.

Newton's Law of Cooling is stated as a special case of Stefan-Boltzmann Law where the temperature difference is very small and is formulated as ##\frac {dQ}{dt} = k(T_2 - T_1)##.

I feel that the three must be somehow interrelated, am I correct in assuming this? If so, how?

3. Lastly is emissivity the same as Stefan's constant or is it ## e * \sigma## where ##e## varies, depending on the material?

Thank you!
 
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Hi JC
1. the object has a net absorption of radiation
2. e represents emissivity, σ represents the Stefan - Boltzmann constant
3. ε = 1 for a black body. For all real materials, it varies from 0 to 1, and can be frequency dependent.

Newton's Law of cooling - if the temperature difference is large, then radiation effects should be taken into account
 
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  • #3
1. So ##H## represents the rate of absorption? (If so, shouldn't heat absorption have a positive sign and hence rate of heat absorption should also have a positive sign?)
2. Thanks that makes it clear!
3. So, it is safe to say that Stefan-Boltzmann's law could be used in place of the other two formulas while the other two are special cases (for small T differences we have Newton's Law of Cooling and the formula of conduction is when heat transfer is occurring within a substance). Thus Stefan-Boltzmann's law could be used to find the rate of heat transfer in all cases?
 
  • #4
JC2000 said:
1. So ##H## represents the rate of absorption? (If so, shouldn't heat absorption have a positive sign and hence rate of heat absorption should also have a positive sign?)
2. Thanks that makes it clear!
3. So, it is safe to say that Stefan-Boltzmann's law could be used in place of the other two formulas while the other two are special cases (for small T differences we have Newton's Law of Cooling and the formula of conduction is when heat transfer is occurring within a substance). Thus Stefan-Boltzmann's law could be used to find the rate of heat transfer in all cases?
1. In which direction you assign heat flow, in or out, would be case dependent.
Example - the sun outputs X amount of radiation, so one would consider that a positive value for the sun.
the Earth receives Y amount of heat flux, so one would consider that as a positive value for the earth.

3. probably not. Conduction and convection are heat transfers by contact, not by radiation.
 
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What is the Stefan-Boltzmann Law?

The Stefan-Boltzmann Law is a physical law that describes the relationship between the temperature of an object and the amount of radiation it emits. It states that the total energy emitted per unit surface area of an object is proportional to the fourth power of its absolute temperature.

How does the Stefan-Boltzmann Law work?

The law states that the total energy emitted (E) per unit surface area of an object is given by E = σT^4, where σ is the Stefan-Boltzmann constant and T is the absolute temperature of the object in Kelvin. This means that as the temperature of an object increases, the amount of radiation it emits also increases significantly.

What is the significance of the Stefan-Boltzmann Law?

The Stefan-Boltzmann Law is significant because it helps us understand the behavior of thermal radiation and the relationship between an object's temperature and the amount of energy it emits. It is also used in various fields such as astrophysics, engineering, and climate science to calculate and predict thermal radiation.

How does the Stefan-Boltzmann Law apply when the surroundings are hotter?

When the surroundings are hotter than the object, the object will emit less radiation compared to when the surroundings are cooler. This is because the object is absorbing more radiation from its surroundings, which reduces the net amount of radiation it emits. However, the Stefan-Boltzmann Law still applies, and the object's radiation will increase as its temperature increases.

What are some real-life applications of the Stefan-Boltzmann Law?

The Stefan-Boltzmann Law has various real-life applications, including measuring the surface temperature of stars, calculating the heat loss of buildings, and predicting the thermal radiation from Earth's atmosphere. It is also used in the design of solar panels, as it helps determine the amount of energy they can absorb and convert into electricity.

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