1. Announcements Observing on the roof of Van Allen Hall has started and will run Tuesday to Thursday from 9-11 pm this week. The first hour exam will be on Friday, September 17.

2. Temperature and Color, Classifying Stars Spectrum of light How the eye sees color Temperature and color/spectrum Colors/spectra of stars Classifying stars Reading: sections: 16.5-16.6, 6.2

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

4. How your eye sees light and color

5. Rods and cones on the retina sense light

6. 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

7. Sensitivity of cones

8. 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.

11. What can we learn from a star’s color? The color indicates the temperature of the surface of the star. The same is true for the filament in a light bulb or any other hot object. In general, we call radiation from a hot body `black body’ radiation (do demonstration 6B40.10).

12. Wien’s law Cooler objects produce radiation which peaks at longer wavelengths (redder colors), hotter objects produce radiation which peaks at shorter wavelengths (bluer colors).

13. A star’s color depends on its surface temperature Spectrum demonstration 6B40.55

14. Stars are assigned a `spectral type’ based on their spectra The spectral classification essentially sorts stars according to their surface temperature The spectral classification also uses spectral lines, which will discuss on Friday

15. Spectral type Sequence is: O B A F G K M O type is hottest (~25,000K), M type is coolest (~2500K) Star Colors: O blue to M red Sequence subdivided by attaching one numerical digit, for example: F0, F1, F2, F3 … F9 where F1 is hotter than F3. Sequence is O … O9, B0, B1, …, B9, A0, A1, … A9, F0, … Useful mnemonics to remember OBAFGKM: –Our Best Astronomers Feel Good Knowing More –Oh Boy, An F Grade Kills Me –(Traditional) Oh, Be a Fine Girl (or Guy), Kiss Me

16. The spectrum of a star is most determined by 1.The temperature of the star’s surface 2.The star’s distance from Earth 3.The density of the star’s core 4.The luminosity of the star

17. Classifying stars We now have two properties of stars that we can measure: –Luminosity –Color/surface temperature Using these two characteristics has proved extraordinarily effective in understanding the properties of stars – the Hertzsprung- Russell (HR) diagram

18. HR diagram

19. Originally, the HR diagram was made by plotting absolute magnitude versus spectral type Now, it’s better to think of the HR diagram in terms of physical quantities: luminosity and surface temperature

20. If we plot lots of stars on the HR diagram, they fall into groups

21. These groups indicate types of stars, or stages in the evolution of stars

22. Luminosity classes Class Ia,b : Supergiant Class II: Bright giant Class III: Giant Class IV: Sub-giant Class V: Dwarf The Sun is a G2 V star