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Homework #9: Do not turn this in. I will post my solutions so that you can check your work.
That's all for homework #9.
- problem 6.3. This problem illustrates how the partition function Z is a dynamic thing that depends on the temperature.
- problem 6.5
- problem 6.7. In this problem, referring to Figure 6.2, you should see that the energy levels are given by the standard Bohr approximation, En=(-)13.6eV/n2. Note the degeneracies here are given by gn=2n2. Thus g1=2*12=2, g2=2*22=8 and g3=2*32=18 for n=1 (ground state), n=2 (first excited) and n=3 (second excited) states, respectively. Just as I discussed in class.
- Consider the hydrogen-like atom carbon-V in stellar atmospheres. Carbon-V is simply a carbon atom with 5 of its electrons ripped off by the extreme heat, and one electron remaining to jump around the usual energy levels. Calculate the temperature at which you would expect a ratio of 1/7 for a carbon-V atom being in its n=8 state to being in its n=7 state. Remember to take degeneracy into account.
- problem 6.12. Note: If this problem doesn't make an impression on you about the universe, and how we can use what you are learning to discern something amazing about the universe, then you just don't have a pulse.