1. ASTR 1102-002 2008 Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture11]

2. Plot “L vs. T” for 27 Nearest Stars Data drawn from Appendix 4 of the textbook.

3. L and T appear to be Correlated Nearest Stars

4. L and T appear to be Correlated A few of the brightest stars in the night sky

5. Hertzsprung-Russell (H-R) Diagram

6. Chapter 19: Stellar Evolution: On & after the Main Sequence

7. Apply the “Age” Concept to Other Stars How long can other stars live? –t age = fMc 2 /L –(t age /10 10 years) = (M/M sun )/(L/L sun )

8. Apply the “Age” Concept to Other Stars

9. How does a Star’s Structure Change as it Ages (Evolves)?

10. Open Cluster: NGC 290

11. Hertzsprung-Russell (H-R) Diagram

12. Pleiades Star Cluster (age approximately 50 million years) Figure 18-19

13. Figure 19-9 Post-main-sequence Evolutionary Tracks:

14. H-R Diagram for Open Clusters Figure 19-14

15. Figure 19-11

16. Globular Cluster M10 Figure 19-12

17. Globular Cluster M55

18. Globular Cluster M10 Figure 19-12

19. Chapter 18: The Birth of Stars

20. Dust in Spiral Galaxies Figure 18-8

21. A Dark Nebula in Our Galaxy Figure 18-4

22. Figure 18-10 Pre-main-sequence Evolutionary Tracks:

23. Figure 18-18 NGC 2264: A Very Young Cluster

24. Figure 19-10