1. Light, Color, Spectral Lines Spectrum of light Photon energy Atomic structure Spectral lines Elements in stars How the eye sees color Temperature and color/spectrum Colors of stars

2. Electromagnetic spectrum The “spectrum” of a particular star is how much light it produces at each wavelength.

3. Photon energy Up to now, we have been discussing the wavelength of light as determining it color However, light comes in discrete packets called photons and the energy of each photon is set by its color or wavelength From Einstein, we known that the photon energy is inversely proportional to its wavelength

4. Photon energy

5. Hydrogen atom Electron orbits around nucleus

6. Electron orbits From quantum mechanics, only certain orbits are allowed. Each orbit has a specific energy.

7. How atoms emit light

8. The emitted photon has an energy which is exactly the energy difference between the orbits that the electron had before and after. Because only certain energies are allowed for the electron orbits, only certain energies of photons can be produced. We call these the spectral lines of hydrogen.

9. Spectral lines of hydrogen The length of each arrow determines the energy and therefore the wavelength of the photon emitted.

10. Spectral lines Each element (hydrogen, helium, neon, mercury, iron, …) has its own particular set of energy levels and its own set of spectral lines. Do demonstration (7B10.10)

11. Uses of spectral lines Because each element has it own unique pattern of spectral lines, the spectral lines from stars can be used to determine the composition, or the relative number of atoms of each elements, of the stars

12. Kirchoff’s laws A hot solid, liquid, or dense gas produces a continuous spectrum. A thin gas in front of a cooler background produces an emission line spectrum. A thin gas in front of a hot source imprints absorption lines on the spectrum. This is mainly what we see from stars.

13. Absorption spectrum of a star

14. A object’s color depends on its surface temperature Wavelength of peak radiation: Wien Law max = 2.9 x 10 6 / T(K) [nm]  Spectrum demonstration 6B40.10 or.55

15. How your eye sees light and color

16. Rods and cones on the retina sense light

17. Rods and cones Cones are color sensors There are cones for red, green, and blue The color ones perceives depends on the firing rates of the red vs. green vs. blue cones Cones need relatively bright light to work Rods give finer, more detailed vision Rods can work with less light At night, color vision is less effective because only the rods function

18. Sensitivity of cones

19. A star will produce light overlapping the response of all three cones. The color of the star depends on how strong its spectrum is in the ranges covered by the different cones.

22. UBV Observationally, we measure colors by comparing the brightness of the star in two (or more) wavelength bands. This is the same way your eye determines color, but the bands are different.

23. What can we learn from a star’s color? The color indicates the temperature of the surface of the star.

24. The ratio of fluxes in two bands translates to the difference in magnitudes, or a color, e.g. B – V = m B – m V. Stellar temperature follow an approximate, empirical relation: T ~ 9000 K/[(B-V) + 0.93]