Pre-Laboratory Exercises 2-8 PHYS UN1292 1. What is the wavelength of emitted light if an electron in a hydrogen atom makes a transition from n; = 3 to ny = 1? 2. If you look at the light of an object at high temperature (e.g., a normal light bulb), you will find that it usually emits a continuous spectrum without any gaps or lines in it. But if you look at the spectrum of the sun (or another star), you will find a continuous spectrum that has a number of sharp black lines, so no (or almost no) light of that frequency reaches you; the light of that frequency is missing in the spectrum. These black lines are at exactly the same positions where you would see the colored lines in emission spectra (that is what we do in lab) of the elements present on the sun. For example since hydrogen is present on the sun we find black line at the wavelengths in the hydrogen emission spectrum. Can you give a short explanation of how we get these inverse spectra (compared to the ones we see in the lab from emission spectra) from the sun? Hint: Think about the relationship between emission and absorption. D2