schroeder introduction to thermal physics solutions 2.42

What does the partition function partition?ģ. On problem 6.10, calculate the wavelength of a photon (in micron units) that corresponds to an excitation from the ground state to the first excited state what part of the electromagnetic spectrum is this photon in?ġ. On problem 6.10, you can calculate the partition function by adding terms, and can quit adding terms when they are so small that they don't contribute anymore. Boltzmann's constant is given in eV/K on page 402. In 6.3 it is a good idea to plot the partition function as a function of (kT/epsilon) too so you can see the functional form. You can do both with one for extra credit. (someone send me a C-code or other example too.) Your results should look something like this:

You can use Mathematica or Maple and do the derivatives using these programs, or do so numerically using other programs such as Fortran or Matlab, etc. You will have to figure out how to take the derivative for heat capacity calculation from energy. Note thatĬomputational problem concerning the heat capacity of para and ortho hydrogen. Rotational partition function at low temperature. Problem 6.24 helps with the rotational partition function for O2 at room temperature. Then the partition function for O2, and obtain the entropy and chemical potential from it. Speed of O2 molecules at room temperature. How is the Debye theory of solids different from the Einstein theory of solids? How many food calories would you need to eat to replace the energy you would lose in 12 hours due to black body radiation emission if you did not receive infrared energy from the environment.Ĩ. What is the value of the Stefan Boltzmann constant? Use it to estimate how much radiative power your body would emit (neglecting clothes). How does the entropy of a black body relate to the number of photons in a black body?ħ. How does the total energy density of a black body vary with temperature? Think about the Earth at a lowly 285 K, the Sun exterior at 5800 K, and the Sun interior at around 15 million K.Ħ. What keeps matter from collapsing under the huge electrostatic forces that try to pull electrons and protons together?ĥ. Why is it that quantum statistics are different for particles called Bosons and Fermions?ģ. How is the Gibbs factor different from the Boltzmann factor?Ģ.

Read chapter 7, carefully, with concentration, effort, and strength. electrons in a metal and photons from the sun. the heat capacity when you sum to n=15 in the partition function. The heat capacity when you sum to n=12 in the partition function, 4. the heat capacity when you sum to n=10 in the partition function, 3. the harmonic oscillator solution when En=Epsilon*n, 2. Make a plot similar to the one we did for that problem. You can modify the code we used for problem 6.26 and apply it here for this problem.

Heat capacity of the anharmonic hydrogen molecule, and interpretation of results.

Schroeder introduction to thermal physics solutions 2.42