AGB stars as laboratories for nuclear physics

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Aubrey Parks
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1 AGB stars as laboratories for nuclear physics John Lattanzio with Amanda Karakas 1, Lisa Elliott, Simon Campbell, Maria Lugaro 2, Carolyn Doherty Centre for Stellar and Planetary Astrophysics, Monash University,Australia 1 now at Centre for Computational Astrophysics, St Marys University, Halifax 2 now at Institute of Astronomy, Cambridge University

3 AGB Nucleosynthesis 1. He Flashes and hot bottoms etc 2. C stars 3. S-process elements F 25 Mg and 26 Mg (and Al isotopes) 23 Na 7 Li 14 N 9. etc

4 HR Diagram (Globular Cluster) AGB (Second giant branch) Horizontal Branch (core He burning) RGB (first giant branch) Blue Stragglers Main sequence (H burning) White Dwarfs

5 HR Diagram (Globular Cluster) Here be monsters Giants complicated! Friendly Main Sequence Stars Graveyard

6 Nucleosynthesis

7 Z = number of protons Chart of the Nuclides: The big boys/girls periodic table N = number of neutrons

8 Why was it OK to have H, He and Z? For the structure we need the energy generation Burning H to He or He to C covers most of HRD! So we can make accurate models with only H and He burning Very few species needed Me: H, He 3, He 4, C 12, N 14 and O 16

9 H burning PP chains or CNO cycle(s) PP chains: pure H gas is all that s needed CNO cycles require CNO as catalysts

10 First reaction: p + p D 2 + γ D 2 + p He 3 + γ He 3 + He 3 He 4 + 2p PP Chains

11 Branching reaction: PP Chains He 3 + He 4 Be 7 + γ Be 7 + p B 8 He 4 + He 4 Be7 + e Li 7 Li 7 + p He 4 + He 4

12 CNO Cycles: First step is CN cycle C p C 12 + He 4

13 CNO Cycles

14 And then things went CRAZY!

15 Who were the trouble makers? Pre-solar meteorite grains Pieces of stars! In the lab!

16 The Nuclear Network we now use 74 species 506 reactions

17 Basic Stellar Evolution: Mass is the key! no Die as a Brown Dwarf Burn H? yes Die as a He White Dwarf no Burn He? yes no Die as a CO White Dwarf Burn C? yes Die as a O-Ne-Mg White Dwarf no More burning? yes Wolf-Rayet SN II

18 Basic Stellar Evolution: Mass is the key! Mass Initial Mass Function: N ~ M -2.3 SN & WR AGB stars Don t burn more O-Ne-Mg WD Burn more Don t burn C C-O White Dwarf Burn C Don t burn He He White Dwarf Burn He Don t burn H Brown Dwarf Burn H

19 Basic Stellar Evolution at M=1 and 5 Basic Evolution: M=1 & 5

20 H burning summary at M=1

21 End of H burning: He ignition

22 Following He exhaustion: AGB Evolution

23 Early AGB Evolution: Second Dredge-Up

24 Thermally pulsing AGB phase Deep convective Envelope Thin radiative zone H-burning shell He-rich intershell He-burning shell CO core

25 AGB Evolution

26 AGB evolution: M = 6.5, Z=0.02

27 AGB Evolution Energy Sources

28 AGB Evolution Shell Movement

29 Dredge-Up Parameter: λ

30 AGB Evolution Mixing Zones

31 Anatomy of a Thermal Pulse He - C 14 N to 22 Ne M>3: 22 Ne to 25 Mg and 26 Mg

32 AGB movies

33 M MS S C(N) Add C at each drede-up episode Eventually C/O > 1 M star turns into a C star Fits observations (pretty much )

34 Neutron capture: the s and r β + decay: p n + ν + β + processes Valley of beta stability β - decay: n p + ν + β -

35 S-process elements in AGB stars Neutron capture on Fe: Sr, Y, Zr, Ba, Kr etc

36 Mg isotopes in field stars Gay and Lambert found some enhancements in heavy isotopes Does not fit SN models

37 Anatomy of a Thermal Pulse He - C 14 N to 22 Ne M>3: 22 Ne to 25 Mg and 26 Mg

38 Mg 25,26 (and maybe Al 26,27) For T > 300 million (M > 2.5) Al 26 and Al 27 dredged to surface Mg 25 and Mg 26 dredged to surface Another source of neutrons! Ne 22 (α,n)mg 25 Ne 22 (α,γ ) Mg 26 Al 26 and Al 27 made by H shell via proton captures on Mg Al engulfed by convection

39 Intershell abundances: as a function of mass & Z

40 Evolution of the Mg isotopes

41 Massive stars produce most of the galactic magnesium, which is primarily 24 Mg at low Z But 3-6 M sun AGB stars can produce large amounts of the heavy magnesium isotopes (Y. Fenner, A. Karakas, B. Gibson, J. Lattanzio)

42 AGB stars are needed to recover the observed 25,26 M/ 24 Mg ratios at low metallicity Limongi et al. (2002) calculations generate more 25,26 Mg than Woosley & Weaver (1995) (Y. Fenner, A. Karakas, B. Gibson, J. Lattanzio, PASA, 2003)

43 Fluorine Observations show [F/O] correlates with C/O This implicates thermal pulses Complicated - different reaction paths - depends on mass - depends on composition - depends on pulse number

44 Fluorine

45 3. And finally N 15 (α,γ)f Protons made here by Al 26 (n,p)mg O 18 (p,α)n Protons made here by N 14 (n,p)c 14

46 GCE of 19 F Renda et al (submitted) SN, WR and AGB SN & WR x = Milky Way = LMC = ω Cen SN only

47 Sodium 12 C 14 N 22 Ne 23 Na 23 Na 22 Ne 23 Na Note: some 23 Na is primary and some is secondary!

48 Making Li

49 Making Li

50 Primary Nitrogen in the early Universe Various observations 9eg Lyman alpha clouds) show a primary source of N in the early Universe AGB stars again? Primary C is produced by dredge-up (H He C) CNO cycles make N 14 from C and O Thus HBB makes Primary N 14

52 Summary of Nucleosynthesis in AGB stars Dredge-up increases: C, Ne 22, Mg 25, Mg 26 H shell and HBB (M>4) burns: 1) C and O into N: O down and N up 2) Ne22 into Na23: Na up 3) Mg25 and Mg26 made: Mg 25,26 increased More massive stars (M > 6?): 1) Mg24 burned into Al27: Mg 24 down Al 27 up Overall 1) Increases in N, Na, heavy Mg, Al 2) Decreases in O, Mg 24

53 The End?

54 More appropriate for a theorist Play Tom Lehrer Song

The Monash Chemical Yields Project

The Monash Chemical Yields Project Carolyn Doherty (Konkoly Observatory) George Angelou Simon W. Campbell Ross Church Thomas Constantino Sergio Cristallo Pilar Gil Pons Amanda Karakas John Lattanzio Maria