Specific Heat at constant pressure for photon gas

In summary: Method 1 uses a Maxwell relation to show that the heat capacities at constant pressure and volume are equal, while method 2 calculates the heat capacity at constant pressure to be 4/3 times the heat capacity at constant volume. This discrepancy arises because the heat capacity at constant pressure is not a meaningful quantity for this system.
  • #1
sy7kenny
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Homework Statement


A blackbody photon gas is contained within an evacuated cavity ([tex]V = 0.01 m^3[/tex]).
Calculate [tex]C_p[/tex] for the photon gas at T = 1000K

Homework Equations


[tex] C_p - C_v = T(\frac{\partial S} {\partial V}) (\frac{\partial V}{\partial T})[/tex]
[tex] C_v = T(\frac{\partial S} {\partial T}) [/tex]
[tex] S = \frac{16}{3} \frac{\sigma}{c} V T^3 [/tex]
[tex] p = \frac{1} {3} \frac{U}{V}[/tex]
[tex] dU = đ Q - p dV[/tex]

The Attempt at a Solution


I got two different answers for the following methods, please let me know if I am neglecting any assumptions.

Method 1 Maxwell Relation
[tex] C_p - C_v = T(\frac{\partial S} {\partial V}) (\frac{\partial V}{\partial T})[/tex]
[tex] C_v = T(\frac{\partial S} {\partial T}) [/tex]
[tex] C_p = T(\frac{\partial S} {\partial T}) + T(\frac{\partial S} {\partial V}) (\frac{\partial V}{\partial T})[/tex]

then by using the Maxwell relation,
[tex] (\frac{\partial V} {\partial T}) = -(\frac{\partial S}{\partial P})[/tex]
[tex] C_p = T(\frac{\partial S} {\partial T}) -T(\frac{\partial S} {\partial V})(\frac{\partial S}{\partial P})[/tex]
but S does not depend on pressure thus [tex] (\frac{\partial S}{\partial P}) = 0[/tex]
leaving [tex]C_p = T(\frac{\partial S} {\partial T}) = C_v = 16\frac{\sigma}{c}V T^3 [/tex]

Method 2,
Using [tex] p = \frac{1} {3} \frac{U}{V}[/tex],
[tex]U = 3pV[/tex]
[tex]C_v = \frac{\partial U}{\partial T}[/tex]
[tex] dU = đ Q - p dV[/tex]

[tex](đ Q)_p = dU + p dV = 4 p dV = \frac{4}{3} dU[/tex]
[tex]C_p = (\frac{\partial Q}{\partial T})_p[/tex]

which lead to
[tex]C_p = \frac{4}{3} \frac{\partial U}{\partial T} = \frac{4}{3} C_v[/tex]

in short,
method 1 says [tex]C_p = C_v [/tex]
method 2 says [tex]C_p = \frac{4}{3} C_v [/tex]

I am not sure why the two results do not agree. Any help will be appreciated. Thanks!
 
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  • #2
The heat capacity of photon gas at constant pressure is a trick question. It's not well defined, since temperature and pressure cannot be varied independently of each other in this system.
 
Last edited:

Related to Specific Heat at constant pressure for photon gas

What is specific heat at constant pressure for photon gas?

Specific heat at constant pressure for photon gas is a measure of the amount of heat energy required to raise the temperature of a unit mass of photon gas by one degree while keeping the pressure constant.

Why is specific heat at constant pressure important for photon gas?

Specific heat at constant pressure is important for photon gas because it helps us understand the amount of energy needed to increase the temperature of a photon gas, which is crucial in fields such as astrophysics and cosmology.

How is specific heat at constant pressure calculated for photon gas?

The specific heat at constant pressure for photon gas is calculated using the formula Cp = (4/3) * (aT^3), where a is the radiation constant and T is the temperature in Kelvin.

How does specific heat at constant pressure differ from specific heat at constant volume for photon gas?

Specific heat at constant pressure differs from specific heat at constant volume for photon gas because at constant pressure, energy is allowed to escape through expansion and work done by the gas, while at constant volume, energy is not allowed to escape and the work done is zero.

What are the real-world applications of specific heat at constant pressure for photon gas?

Specific heat at constant pressure for photon gas has real-world applications in fields such as astrophysics, cosmology, and materials science. It helps us understand the behavior of photon gas in various temperature and pressure conditions, and is crucial in the study of stars, galaxies, and other astronomical objects.

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