Evolution of the Elements (Primordial and Stellar Nucleosynthesis) Dana S. Balser. Corradi & Tsvetanov

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1 Evolution of the Elements (Primordial and Stellar Nucleosynthesis) Dana S. Balser Corradi & Tsvetanov

2 Cosmic Evolution

3 Contents of the Universe

4 Simulation: Large Scale Structure Volker Springel

5 Simulation: Galaxy Cluster Volker Springel

6 Primordial Nucleosynthesis 2p p H n n H H p H production n H H p H production p H H H H n H production Tritium H p n bottleneck Deuterium Be production Be Li H production Li

7 Primordial Nucleosynthesis Burles et al. (2001)

8 Lyman, Balmer, Series Hydrogen

9 + Hyperfine Transition N= 2 S 1 / 2 F 0 1 N=2 N=1 F=0 Singlet F=1 Triplet MHz (.46 cm ) A x s 1 (16,00 years )

10 4 Observations: Optical Recombination Lines HII regions in metal poor blue compact galaxies Izotov et al. (1999)

11 4 Results Olive & Skillman (2004) Peimbert & Peimbert (2002) Yp [mass] Reference (0.0012) Izotov et al. (2007) (0.0028) Peimbert et al. (2007) (0.009) Olive & Skillman (2004)

12 7Li Observations: Resonance Line Metal poor Halo stars Boesgaard et al. (2005)

13 7Li Results: The Spite Plateau Log(7Li/H) + 12 Reference Spite & Spite (1982) 2.09 (+0.19,-0.1) Ryan et al. (2000) 2.7 (0.1) Melendez & Ramirez (2004) 2.44 (0.18) Boesgaard et al. (2005)

14 Deuterium Observations: Lyman Series Q HS Kirkman et al. (200) O Meara et al. (2001)

15 Deuterium Results D/H Steigman (2007)

16 + Observations: HII Regions HII Regions: M16 Bania et al. (1997)

17 + Observations: PNe PNe: NGC 242 Balser et al. (1997)

18 Results: The Plateau ( /H) 1.1 primordial 0.2 x 10-5 Bania, Rood, & Balser (2002)

19 Cosmic Microwave Background (WMAP) h b x Spergel et al. (2006)

20 Primordial Abundances Izotov et al. (2007) Peimbert et al. (2007) Olive & Skillman (2004) Kirkman et al. (200) Bania, Rood & Balser (2002) Ryan et al. (2000) Boesgaard et al. (2005) Burles et al. (2001) Spergel et al. (2006)

21 Stellar Nucleosynthesis p Li Li e Be 10 7 Be p p H e H p p K x T K x T

22 Evolution of Bania, Rood & Balser (2002)

23 The Problem Daniele Galli

24 Stellar Evolution of : Theory Daniele Galli

25 -D Hydrodynamical and Nucleosynthetic Network 4 2 p Raleigh-Taylor Instability Eggleton et al. (2006)

26 Thermohaline Mixing Low Viscosity High Viscosity Red (lower salinity) Blue (higher salinity) 4 2 p Denissenkov

27 Evolution of Lagarde et al. 2012

28 Fini

29 Evolution of 4 dy/dz = 1.5 Balser et al. (2010)

30 Evolution of Deuterium D/H Steigman (2007)

31 Evolution of Deuterium ( D / H ) ( D / H ) primordial Galactic Wood et al. (2004) Linsky et al. (2008)

32 Evolution of 7Li Spite & Spite (1982)

33 Evolution of 7Li Ryan et al. (2000)

34 Primordial Abundances 4 Steigman (2010)

35 Primordial Abundances D 7 Li Steigman (2010)

36 4: Galactic HII Regions HII Region: S206 Balser (2006) Caplan et al. (2000)

37 Deuterium: Galactic Anticenter Deuterium 27 MHz Hyperfine Transition D / H x10 5 Rogers et al. 2007

38 Internal Gravity Waves Charbonnel & Talon (2005)

39 -D Hydrodynamical and Nucleosynthetic Network 4 2 p Raleigh-Taylor Instability Eggleton et al. (2006)

40 Thermohaline Mixing Charbonnel & Zahn (2007)

41 Search for in Planetary Nebulae NRAO Green Bank Telescope NRAO Very Large Array NAIC Arecibo Telescope NGC 6572 J20 NGC 242 NGC 654 NGC 7009 NGC 6826 NGC 6210 NGC 6891

42 VLA J20 + Spectra Balser et al. (2006)

43 VLA J20 Model /H Balser et al. (2006)

44 GBT NGC hr integration

45 GBT (NGC NGC654 + NGC6826) 180. hr integration

46 Arecibo (NGC NGC6891)

47 No Mixing in NGC242 + line at 8665 MHz C III] multiplet near 1908 A /H 2-5 x C/ 1 /H 2-5 x 10 C 8 12 C/ 1 C 8 12 C/ 1 C 8 Balser et al. (1999) Palla et al. (2002)

48 Galactic Evolution of : Theory Steigman & Tosi (1992)

49 Rotational Mixing in Stars mixing standard meridional circulation driven by internal rotation might lead to the mixing of CNO-processed material of a red giant star. Sweigart & Mengel (1979) 96% of low-mass stars do experience an extra-mixing process on the RGB Charbonnel & do Nascimento (1998) meridional circulation does not lead to enough mixing to explain the abundance anomalies Palacios et al. (2006) Charbonnel (1995)

50 Thermohaline Mixing 4 2 p Cantiello