Exam #1. mean = 64 median = 65 std dev = 18.1
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1 Exam # mean = 64 median = 65 std dev = 8.
2 Exam # mean: 6. median: 6 mean: 6.5 median: 7 mean = 0.9 median: 2 mean: 2.9 median: 4 hardest question mean:.3 median: 4 easiest question mean: 6.2 median: 6
3 Star Formation Unfortunately, no good quantitative theory to predict star formation rate or stellar mass distribution! IMF = Initial Mass Function N(m)dm = # stars in mass range m to m+dm N(m)dm (m/msun) -α α = 2.35 (Salpeter IMF) Is it universal?
4 Star Formation Birth Sequence trigger kicks off process in an interstellar gas cloud cloud fragments and collapses [MJ and RJ ] early collapse is isothermal; E radiated away interior becomes adiabatic; E trapped so T rises protostellar core forms (~5AU) w/ free-falling gas above dust vaporizes as T increases
5 Star Formation R 0 3 R log( luminosity, L ) R R 0. R 0-2 R 0-3 R 5M 9M 6M protostars 5M 2M M 0.5M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
6 Star Formation R 0 3 R log( luminosity, L ) R R 0 Which stellar structure equation has just been R 0-2 R 0-3 R 5M 9M DISCUSSION QUESTION satisfied by these protostars? A) equation of state B) hydrostatic equilibrium 6M 5M 2M M 0.5M protostars C) mass continuity D) temp gradient 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
7 Star Formation R 0 3 R log( luminosity, L ) R R 0. R 0-2 R 0-3 R 5M 9M 6M protostars 5M 2M M 0.5M Hayashi limit O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
8 Star Formation Protostars T Tauri star artist s rendition
9 Star Formation Protostars DISCUSSION QUESTION T Tauri star What will a spectral line emitted by the T Tauri star look like? A) C) B) v=0 D) v=0 artist s rendition v=0 v=0
10 Star Formation Protostars T Tauri star artist s rendition P Cygni profile
11 Star Formation R 0 3 R log( luminosity, L ) R R 0. R 0-2 R 0-3 R 5M 9M 6M 5M 2M M 0.5M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
12 0 R The Main Sequence R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R MAIN SEQUENCE 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
13 0 R The Main Sequence R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R MAIN SEQUENCE 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
14 The Main Sequence M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M M 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
15 Low-Mass Stars - Main Sequence M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M M 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
16 Low-Mass Stars - Main Sequence Main Sequence Phase on Main Sequence ~ 0 0 M/L L = 4 x 0 33 ergs/s solar constant Age = 4.6 billion yrs (.4 x 0 7 secs) Total E = 6 x 0 50 ergs (fusion is only source capable of this energy) How much E has the sun produced?
17 Low-Mass Stars - Main Sequence H as Stellar Fuel: proton-proton chain 2 ) H+ H H+e + + ν 2 3 2) H+ H 2He+ γ ) He+ He He+2 H E = mc 2 = [0.05 x 0-24 g] x [3 x 0 0 cm/s] 2 = 4 x 0-5 ergs For sun: E = [0.007 x 0. (2x0 33 g)] x [3 x 0 0 cm/s] 2 =.3x0 5 ergs 2 2 4H He + E (Δm=0.05 x 0-24 g) mh=.67 x 0-24 g, so Δm/4mH ~
18 Low-Mass Stars - Main Sequence H as Stellar Fuel: proton-proton chain 2 ) H+ H H+e + + ν 2 3 2) H+ H 2He+ γ ) He+ He He+2 H DISCUSSION QUESTION Where did that factor of 4H 0. come He + from? E How could we have derived (Δm=0.05 that value? x 0-24 g) mh=.67 x 0-24 g, so (discuss) Δm/4mH ~ E = mc 2 = [0.05 x 0-24 g] x [3 x 0 0 cm/s] 2 = 4 x 0-5 ergs For sun: E = [0.007 x 0. (2x0 33 g)] x [3 x 0 0 cm/s] 2 =.3x0 5 ergs
19 Low-Mass Stars - Main Sequence H as Stellar Fuel: proton-proton chain 2 ) H+ H H+e + + ν 2 3 2) H+ H 2He+ γ ) He+ He He+2 H E = mc 2 = [0.05 x 0-24 g] x [3 x 0 0 cm/s] 2 = 4 x 0-5 ergs For sun: E = [0.007 x 0. (2x0 33 g)] x [3 x 0 0 cm/s] 2 =.3x0 5 ergs 2 2 4H He + E (Δm=0.05 x 0-24 g) mh=.67 x 0-24 g, so Δm/4mH ~ core H mass (from stellar structure eq ns) 2
20 Low-Mass Stars - Main Sequence Main Sequence Phase on Main Sequence ~ 0 0 M/L L = 4 x 0 33 ergs/s solar constant Age = 4.6 billion yrs (.4 x 0 7 secs) Total E = 6 x 0 50 ergs (fusion is only source capable of this energy) mass with T > 0 million K E=.3 x 0 5 ergs E available lifetime = E loss rate. 3 x 0 5 ergs = ~ 3 x 0 7 s ~ 0 0 yrs 4 x 0 33 ergs/s
21 Low-Mass Stars - Turn-off He as Stellar Fuel: He-C fusion: triple alpha process He+ 2He 4 Be+ γ 4 2 Be+ 2He 6C+ γ equilibrium reaction; 8 Be lifetime ~3x0-6 s! 3He C E =.7 x 0-5 ergs
22 Low-Mass Stars - Turn-off M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M HB M AGB RGB GIANTS subgiant 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
23 Low-Mass Stars - Turn-off M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) 0 4 R GIANTS 0 Why do you think these stars 2 3M might expand when R 0-2 R 0-3 R 0M SEQUENCE M AGB DISCUSSION QUESTION RGB MAIN 6M HB they switch from fusing H to fusing He? subgiant (discuss, then give best answer) 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
24 Low-Mass Stars - Turn-off log( luminosity, L ) M 30M 0 R R 0. R 0-2 R 0-3 R MAIN 0 2 R 6M SEQUENCE 3M 0 3 R The mirror effect Whenever a star has a shell burning source, it appears to act 0M AGB like a mirror. 0 4 HB M GIANTS RGB subgiant 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
25 Low-Mass Stars - Turn-off log( luminosity, L ) M 30M 0 R R 0. R 0-2 R 0-3 R MAIN 0 2 R 6M SEQUENCE 3M 0 3 R The mirror effect Whenever a star has a shell burning source, it appears to act 0M AGB like a mirror. 0 4 expanding core = contracting envelope RGB contracting core = expanding HB envelope M GIANTS subgiant 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
26 Low-Mass Stars - Turn-off log( luminosity, L ) R R 0 envelope expands; M 30M 0. R 0-2 R 0-3 R 0 2 R 0 3 R The mirror effect Whenever a star has a shell burning source, it appears to act 0M AGB like a mirror. 0 4 Best current explanation: MAIN the 6M virial theorem! E kin = SEQUENCE HB GIANTS 3M Epot increases (star stays virialized) M RGB subgiant 0.3M 0.M 2 E pot shell stays put; Ekin ~ constant (to maintain T) core contracting; 0-4 Epot decreases O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
27 Low-Mass Stars - Turn-off log( luminosity, L ) R R 0. R 0-2 R 0-3 R 0 2 R 0 3 R on MS ~ 0 0 M/L Open Clusters <000 stars < 0 pc diameter Pleiades 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
28 Low-Mass Stars - Turn-off log( luminosity, L ) R R 0. R 0-2 R 0-3 R 0 2 R turnoff point 0 0 years 0 3 R Open Clusters <000 stars < 0 pc diameter Globular Clusters ~ stars ~20-00 pc M0 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
29 Low-Mass Stars - Turn-off log( luminosity, L ) R R 0. R 0-2 R 0-3 R 0 2 R turnoff point 0 3 R 0 years Open Clusters <000 stars < 0 pc diameter Globular Clusters ~ stars ~20-00 pc M0 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
30 Low-Mass Stars - Turn-off log( luminosity, L ) R R 0. R 0-2 R 0-3 R 0 2 R turnoff point 0 3 R 0 years Open Clusters <000 stars < 0 pc diameter Globular Clusters ~ stars ~20-00 pc M0 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
31 Low-Mass Stars - Turn-off M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M 0 9 years 0 0 years 0 years M 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
32 From a couple weeks ago Low-Mass Stars - Turn-off M 30M 0 R 0 2 R color 0 3 R log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M 0 9 years 0 0 years 0 years M magnitude 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
33 Low-Mass Stars - Turn-off Main-sequence fitting for cluster distances M 30M. Observe B & V images of cluster stars 0 R 0 2 R color 0 3 R log( luminosity, L ) years 2. Plot color-mag diagram of B-V vs. V R 3. Find main sequence R turnoff & lower MS stars 0-2 R 0-3 R 0M MAIN 0 8 years 4. For the SAME B-V on lower MS, read mv from cluster and MV from H-R diagram 5. Use distance modulus m- M to calculate d 6M SEQUENCE 3M 0 9 years 0 0 years 0 years M magnitude 0.3M 0.M m-m = 5(log(d) - ) O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
34 Low-Mass Stars - Deaths M 30M 0 R 0 2 R PNe 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M HB M AGB RGB GIANTS subgiant 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
35 Low-Mass Stars - Deaths Planetary Nebulae Expanding glowing shell of ionized gas ejected from a red giant at the end of its life. ) Outer layers ejected by strong stellar wind 2) As hot luminous core is exposed it emits UV 3) UV ionizes the ejected layers
36 Low-Mass Stars - Deaths Planetary Nebulae Helix Nebula M57 - Ring Nebula
37 Low-Mass Stars - Deaths M 30M 0 R 0 2 R PNe 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M WHITE DWARFS HB M AGB RGB GIANTS subgiant 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
38 Low-Mass Stars - Deaths White Dwarfs Sirius A & B (AV + WD) Size: ~Earth Density: 0 6 g/cm 3 B-Field (G): G Rotation: minutes Pressure: e - degeneracy F
39 Low-Mass Stars - Deaths White Dwarfs WDs aren t undergoing core fusion; supported by electron degeneracy pressure. Pauli exclusion principle: no 2 e - can be in same state (position & momentum) If all states are full, the gas is degenerate. (as T increases, more states available, P T) (at high density, collisions restricted P ρ) When He-C fusion starts, core is e - degenerate; He flash removes degeneracy. Then as the star contracts in the WD phase, ρ increases, whole star becomes e - degenerate.
40 Low-Mass Stars - Deaths White Dwarf M-R Relation P ρ 5/3 hydrostatic equilibrium ρ M/R 3 P M 2 /R 4 R /M /3
41 Type Ia Supernovae The distance ladder
42 Type Ia Supernovae Type I no hydrogen Type II has hydrogen Ia no H has Si Thermonuclear supernovae : result of a WD exceeding the Chandrasekhar limit
43 Type Ia Supernovae Thermonuclear supernovae : result of a WD exceeding the Chandrasekhar mass
44 Type Ia Supernovae Thermonuclear supernovae : result of a WD exceeding the Chandrasekhar mass
45 Type Ia Supernovae Thermonuclear supernovae : result of a WD exceeding the Chandrasekhar mass Chandrasekhar mass: maximum mass of a star that can be supported by e - degeneracy pressure ~.4M
46 Type Ia Supernovae
47 Low-mass Stellar Evolution M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M WHITE DWARFS M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
48 Massive Stellar Evolution M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M WHITE DWARFS M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
49 Massive Stellar Evolution: MS M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) R 0. R 0-2 R 0-3 R A) years -4 0M MAIN 6M SEQUENCE 3M GIANTS Given the data in the H-R diagram M and the fact that a star s main sequence lifetime ~ 0 0 M/L years, how long do massive WHITE stars stay 0.3M on the 0-2 DWARFS 0.M main sequence? QUICK QUESTION C) years B) 0 0- years D) years O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
50 Massive Stellar Evolution: MS H as Stellar Fuel, v2.0 CNO Cycle
51 Massive Stellar Evolution: MS log( luminosity, L ) M 30M 0 R R 0. R 0-2 R 0-3 R 0 2 R 0 3 R DISCUSSION QUESTION 0 You observe 4 a site with lots of O- and B-type stars MAIN 6M in a nearby galaxy. What might you conclude? SEQUENCE GIANTS 0 2 3M new stars 0 long ago -4 0M A) the site is actively forming stars 0-2 WHITE DWARFS B) the site stopped forming M C) the site has a 0.3M low Jeans mass 0.M D) the site has a large Jeans radius O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
52 Massive Stellar Evolution: MS M 30M 0 R 0 2 R 0 3 R log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 0 years 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
53 Massive Stellar Evolution: Post-MS M 30M 0 R 0 2 R 0 3 R red supergiants log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 0 years 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
54 Massive Stellar Evolution: Post-MS M 30M 0 R 0 2 R 0 3 R? log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M WHITE DWARFS yellow gap 0 9 years 0 0 years 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
55 Massive Stellar Evolution: Post-MS Hayashi limit
56 Massive Stellar Evolution: Post-MS A couple weeks ago Hayashi limit
57 Massive Stellar Evolution: Post-MS Hayashi limit 2003 Teffs Levesque et al. 2005
58 Massive Stellar Evolution: Post-MS Hayashi limit 2005 Teffs Levesque et al. 2005
59 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! log( luminosity, L ) M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 0 years 0 3 R 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
60 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! log( luminosity, L ) M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 3 R Humphreys-Davidson Limit 0 0 years 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
61 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! log( luminosity, L ) M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 3 R Humphreys-Davidson Limit 0 0 years 0 years M GIANTS 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
62 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! < < log( luminosity, L ) < < < < 0-2 < < 60M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 3 R Humphreys-Davidson Limit 0 0 years 0 years M GIANTS 0.3M 0.M very active research area! 0-4 The Conti Scenario O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
63 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! < < log( luminosity, L ) < < < < 0-2 < < 60M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 3 R Humphreys-Davidson Limit Wolf-Rayet types 0 0 years 0 years M GIANTS 0.3M 0.M very active research area! 0-4 The Conti Scenario O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
64 Massive Stellar Evolution: Post-MS Wolf- Rayet stars! < < log( luminosity, L ) < < < < 0-2 < < 60M 30M 0 R 0 7 years R 0. R 0-2 R 0-3 R MAIN 0 8 years 0 2 R 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 3 R Humphreys-Davidson Limit luminous blue variables 0M (Tuesday) 0 0 years 0 years M GIANTS 0.3M 0.M very active research area! 0-4 The Conti Scenario O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
65 Massive Stellar Evolution: Post-MS M 30M 0 R 0 2 R SUPERGIANTS 0 3 R log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 0 8 years 6M SEQUENCE 3M 0 9 years WHITE DWARFS 0 0 years 0 years M GIANTS 0.3M 0.M now what? 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
66 Massive Stellar Evolution: Post-MS Post-MS reactions Fe fusion requires rather than produces energy H He C O Ne Mg Si Fe H fusion: ~0 7 years He fusion: ~0 6 years C fusion: ~300 years O fusion: ~200 days Ne fusion: ~days Mg fusion: ~days Si fusion: ~days
67 Massive Stellar Evolution - Deaths ΔP(r) Δr = -GM(r)ρ(r) r 2 (hydrostatic equilibrium) H He C O Ne Mg Si Fe
68 Massive Stellar Evolution - Deaths ΔP(r) Δr = -GM(r)ρ(r) r 2 (hydrostatic equilibrium) H He C O Ne Mg Si At very high T, Fe core is destroyed by photodisintegration free e - s captured by photodisintegration products; e - degeneracy pressure can no longer help core collapses in a matter of seconds (supersonic speeds)
69 Massive Stellar Evolution - Deaths ΔP(r) Δr = -GM(r)ρ(r) r 2 (hydrostatic equilibrium) HHC NM O S density of inner core exceeds ~ 8 x 0 7 kg m -3 n degeneracy pressure kicks in, repels further collapse core rebounds, sends pressure waves that become a shock wave at sonic speed and propagates outward
70 Massive Stellar Evolution - Deaths ΔP(r) Δr = -GM(r)ρ(r) r 2 (hydrostatic equilibrium) QUICK QUESTION In the tabletop demo, will the smaller block rebound to a max distance of A) H/4 density of inner core exceeds ~ 8 x 0 7 kg m -3 B) H/2 n degeneracy pressure kicks in, repels further collapse core rebounds, sends pressure waves that become a shock wave at sonic speed and propagates outward HHC NM O S C) H D) 2*H
71 Massive Stellar Evolution - Deaths Type I no hydrogen Type II has hydrogen Ia Ib Ic no H has Si II has H H He C O Ne Mg Si Fe
72 Massive Stellar Evolution - Deaths Type I no hydrogen Type II has hydrogen Ia Ib Ic no H has Si no H has He no Si II has H He C O Ne Mg Si Fe
73 Massive Stellar Evolution - Deaths Type I no hydrogen Type II has hydrogen Ia Ib Ic no H has Si no H has He no Si no H no He no Si II has H C O Ne Mg Si Fe
74 Massive Stellar Evolution - Deaths SN 054
75 Massive Stellar Evolution - Deaths supernova remnant SN 054/ Crab Nebula Hubble Space Telescope
76 Massive Stellar Evolution - Deaths SN 572 Tycho s Supernova
77 Massive Stellar Evolution - Deaths supernova remnant SN 572 Tycho s Supernova Chandra X-ray Observatory
78 Massive Stellar Evolution - Deaths SN 987A
79 Massive Stellar Evolution - Deaths SN 987A 79 Hubble Space Telescope
80 Massive Stellar Evolution - Deaths M5 Jan 2005 R. Jay. GaBany
81 Massive Stellar Evolution - Deaths M5 SN 2005cs July 2005 R. Jay. GaBany
82 Massive Stellar Evolution - Deaths M5 SN 20dh June 20 R. Jay. GaBany
83 Massive Stellar Evolution - Deaths A few weeks ago M5 SN 20dh June 20 R. Jay. GaBany
84 Next time: weird stars M 30M 0 R 0 2 R SUPERGIANTS 0 3 R log( luminosity, L ) years R 0. R 0-2 R 0-3 R 0M MAIN 6M SEQUENCE 3M M Why is it never this simple? WHITE DWARFS GIANTS years DISCUSSION QUESTION 0 9 years 0 0 years 0 years 0.3M 0.M 0-4 O B A F G K M 30,000 0,000 6,000 3,000 log( temperature, K)
Ay 20 - Lecture 9 Post-Main Sequence Stellar Evolution. This file has many figures missing, in order to keep it a reasonable size.
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