1	Everything you always wanted to know about stars… Material from Chapters 8 and 9 in Horizons by Seeds
2	The Spectra of Stars
3	The Balmer Thermometer Balmer line strength is sensitive to temperature:
4	Measuring the Temperatures of Stars
5	Spectral Classification of Stars (I)
6	Spectral Classification of Stars (II)
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11	Distances to Stars
12	The Trigonometric Parallax
13	Intrinsic Brightness
14	Intrinsic Brightness / Flux and Luminosity
15	The Size (Radius) of a Star
16	Example:
17	Organizing the Family of Stars: The Hertzsprung-Russell Diagram
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20	Radii of Stars in the Hertzsprung-Russell Diagram
21	Luminosity Classes
22	Luminosity effects on the width of spectral lines
23	Examples: Our Sun: G2 star on the main sequence: G2V Polaris: G2 star with supergiant luminosity: G2Ib
24	Binary Stars
25	The Center of Mass
26	“Placeholder” on Masses We can get masses of stars by measuring how they move in binary systems according to Newton’s Law of Gravitation. I’ll save some of the details for exo-solar planets session. Plenty of other things to cover right now…
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29	Surveys of Stars
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31	A Census of the Stars
32	The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky.
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34	Three kinds of nebulae
35	2) Reflection Nebulae
36	Emission and Reflection Nebulae
37	3) Dark Nebulae
38	Interstellar Reddening
39	Interstellar Absorption Lines
40	Structure of the ISM HI clouds:
41	The Various Components of the Interstellar Medium
42	Shocks Triggering Star Formation
43	The Contraction of a Protostar
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45	Evidence of Star Formation
46	Protostellar Disks and Jets – Herbig-Haro Objects
47	Protostellar Disks and Jets – Herbig-Haro Objects (II)
48	Herbig-Haro 34 in Orion Jet along the axis visible as red Lobes at each end where jets run into surrounding gas clouds
49	Motion of Herbig-Haro 34 in Orion Can actually see the knots in the jet move with time In time jets, UV photons, supernova, will disrupt the stellar nursery
50	Globules
51	The Source of Stellar Energy
52	The CNO Cycle
53	Fusion into Heavier Elements
54	Hydrostatic Equilibrium
55	Hydrostatic Equilibrium (II)
56	Stellar Models
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58	Lifetime on Main Sequence L µ M^3.5T µ fuel / L = M/M^{3.5 =} M^-2.5 Example: M=2 M_Sun L = 11.3 L_SunT =1/5.7 T_Sun
59	The Deaths and End States of Stars Material from Seeds chapters 10-11
60	The End of a Star’s Life
61	Evolution off the Main Sequence: Expansion into a Red Giant
62	Expansion onto the Giant Branch
63	Degenerate Matter
64	Red Giant Evolution
65	Evidence for Stellar Evolution: Star Clusters
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67	Estimating the Age of a Cluster
68	Red Dwarfs
69	Sunlike Stars
70	White Dwarfs
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72	The Chandrasekhar Limit
73	The Final Breaths of Sun-Like Stars: Planetary Nebulae
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75	Planetary Nebulae
76	A Gallery of P-N from Hubble
77	Mass Transfer in Binary Stars
78	Recycled Stellar Evolution
79	White Dwarfs in Binary Systems
80	Nova Explosions
81	Recurrent Novae
82	The Fate of our Sun and the End of Earth Sun will expand to a red giant in ~ 5 billion years Expands to ~ Earth’s orbit Earth will then be incinerated! Sun may form a planetary nebula (but uncertain) Sun’s C,O core will become a white dwarf
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84	The Deaths of Massive Stars: Supernovae
85	The Crab Nebula–Supernova from 1050 AD Can see expansion between 1973 and 2001 Kitt Peak National Observatory Images
86	Supernova Remnants
87	The Famous Supernova of 1987: Supernova 1987A
88	Observations of Supernovae
89	Type I and II Supernovae
90	Neutron Stars
91	Discovery of Pulsars
92	The Crab Pulsar
93	The Crab Pulsar
94	Light curves of the Crab Pulsar
95	The Lighthouse Model of Pulsars
96	Images of Pulsars and other Neutron Stars
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98	Pulsar Planets
99	Black Holes
100	Escape Velocity
101	The Schwarzschild Radius
102	Schwarzschild Radius and Event Horizon
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104	“Black Holes Have No Hair”
105	The Gravitational Field of a Black Hole
106	General Relativity Effects Near Black Holes
107	General Relativity Effects Near Black Holes (II)
108	General Relativity Effects Near Black Holes (III)
109	Observing Black Holes
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111	Gamma-Ray Bursts (GRBs)