Stellar Structure and Evolution pp 102-106 | Cite as

# The Ideal Gas with Radiation

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## Abstract

For an ideal gas consisting of with

*n*particles per unit volume that all have molecular weight*μ*, the equation of state is$$ P = nkT = \frac{\Re }{\mu }\rho T, $$

(13.1)

*ϱ*=*nμm*_{n}(*k*= 1.38 × 10^{-16}erg K^{-1}= Boltzmann constant; ℜ =*k/m*_{ u }= 8.31 × 10^{7}erg K^{-1}g^{-1}= universal gas constant; m_{u}= 1 amu = 1.66053 × 10^{-24}g = the atomic mass unit). Note that we here use the gas constant with a dimension (energy per K and per*unit mass*) different from that in thermodynamic text books (energy per K and per mole). This has the consequence that here the molecular weight*m*is dimensionless (instead of having the dimension mass per mole); it is simply the particle mass divided by 1 amu.## Keywords

Free Electron Radiation Pressure Dimension Mass Deep Interior Helium Nucleus
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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© Springer-Verlag Berlin Heidelberg 1990