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Astrophysical origin of the solar Zinc

Astrophysical origin of the solar Zinc. Marco Pignatari Roberto Gallino. Isotopic composition of solar Zn:. Zn64 = 48.6 % Zn(sun) Zn66 = 27.9 % Zn(sun) Zn67 = 4.1 % Zn(sun) Zn68 = 18.8 % Zn(sun) Zn70 = 0.6 % Zn(sun). 64 Zn = 48.6 % Zn(sun) 66 Zn = 27.9 % Zn(sun)

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Astrophysical origin of the solar Zinc

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  1. Astrophysical origin of the solar Zinc Marco Pignatari Roberto Gallino

  2. Isotopic composition of solar Zn: Zn64 = 48.6 % Zn(sun) Zn66 = 27.9 % Zn(sun) Zn67 = 4.1 % Zn(sun) Zn68 = 18.8 % Zn(sun) Zn70 = 0.6 % Zn(sun) 64Zn = 48.6 % Zn(sun) 66Zn = 27.9 % Zn(sun) 67Zn = 4.1 % Zn(sun) 68Zn = 18.8 % Zn(sun) 70Zn = 0.6 % Zn(sun)

  3. Theoretical prediction for evolution of [Zn/Fe] vs [Fe/H] in the galaxy Timmes Woosley & Weaver 1995 [Zn/Fe] = log(Zn/Fe) – log(Zn/Fe)sun [Fe/H] = log(Fe/H) – log(Fe/H)sun

  4. Trend of [Zn/Fe] vs [Fe/H] in the galaxy for unevolved stars SNIa contribution Primary like Secondary like [Zn/Fe] = log(Zn/Fe) – log(Zn/Fe)sun [Fe/H] = log(Fe/H) – log(Fe/H)sun

  5. Astrophysical origin of Zn: • 1. AGB stars? • 2. SNIa? • 3. SNII?

  6. 1. Contribution by AGB stars (main s-component)(Travaglio et al. 1999)

  7. Z β+-decay 9.4h 78.3h 68.3m 69 21.15m 71 Ga Zn 9.13h 38.1m 64 244d 66 67 68 56m 70 Cu 3.4h 9.74m 63 12.70h 65 5.1m 61.9h Ni 60 61 62 100a 64 2.52h 54.6h 59 5.72a 1.65h Co β--decay 58 45.1d 1.5e6a 6.0 m Fe A

  8. 2. Contribution from SNIa ~ 5 %as 64Zn (64Ge, 64Ga) 64Zn is produced by SNIa as much as 0.2 Fe L. Piersanti (priv. comm.) Assuming that 2/3-1/2 Fe(sun) has been produced in SNIa… Zn(SNIa) ~ 6-5 % Zn(sun) 64Zn(sun) = 48.6 % Zn(sun)

  9. 3. Contribution from SNII to solar Zn Primary like Secondary like α-process, ν-wind s-process, Weak sr(p)-process

  10. Primary contribution [Zn/Fe] ~ 0.05

  11. Spectroscopic observations from Halo and Intermediate stars (very metal poor stars not included) (Sneden et al. 1991, Mishenina et al. 2002) [Zn/Fe] ~ 0.05 Zn(pr.) ~ 40-56 % Zn(sun) SNII produced 1/3-1/2 of Fe(sun) Assuming that all primary-like Zn component has been produced by SNII

  12. Primary-like Zn isotopes: • 64Zn: Primary-like isotope. It’s produced by α-rich freezout and ν-wind in the deepest layers (WW95, Woosley et al. 1994, Woosley & Hoffman 1996). • 66Zn: Its primary-like component has been produced by α-rich freezout and ν-wind in the deepest layers ( Woosley & Hoffman 1992).

  13. Post-Supernova composition (yields) 70Zn overproduced*2 M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  14. Pre-Supernova and Post-Supernova composition 66Zn Convective shell C-burning 64Zn He-burning M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  15. Post-Supernova composition (26000 s) Unstable isotopes contribution 64Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  16. Post-Supernova composition (26000 s) Unstable isotopes contribution 66Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  17. Principal isotopes (pre-supernova): M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  18. Pre-Supernova and Post-Supernova composition 66Zn 64Zn M=15 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  19. Secondary-like component to Zn isotopes: • 64Zn: Its secondary-like component is produced by both preSN He-burning (WW95) and C-burning weak sr(p)-process. It is negligible respect to the primary-like component. • 66Zn: Its secondary-like component is produced by both preSN He-burning and C-burning weak sr(p)-process. Uncertain relative weight of the two components.

  20. 67Zn: Secondary-like isotope. It’s produced by both preSN C-burning (~ 70 %) and He-burning (~ 30 %). • 68Zn: Secondary-like isotope. Similar to 67Zn + small postSN contribution at the r-peak. • 70Zn: Strongly produced by SNII, in particular by postSN He-burning and in the r-peak region (see production factors in WW95).

  21. Pre-Supernova and Post-Supernova composition 67Zn 68Zn 70Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  22. Post-Supernova composition (26000 s) Unstable isotopes contribution 67Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  23. Post-Supernova composition (26000 s) Unstable isotopes contribution 68Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  24. Post-Supernova composition (26000 s) Unstable isotopes contribution 70Zn M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  25. Pre-Supernova and Post-Supernova composition 67Zn 68Zn 70Zn M=15 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  26. Post-Supernova production factor M=25 Msun, Z=Zsun (Nucl. Data Page, A. Heger)

  27. Total secondary-like contribution to the solar Zn by SNII: 2/3-1/1 66Zn(sun) 67Zn(sun) 68Zn(sun) ~ 40÷50 % Zn(sun)

  28. SNII Primary-like contribution to solar Zn ~ 40-56 % Secondary-like contribution to solar Zn ~ 40-50 % SNII produced the main part of solar Zn (80-100 %)

  29. Conclusions • SNII produced the main part of solar Zinc, the remnant is produced by SNIa (as 64Zn) and AGB stars. • SNII contribution is divided in two component: the first one is primary-like (as 64Zn and 66Zn), produced by α-process and ν-wind, the second one is secondary-like (as 66Zn, 67Zn, 68Zn) produced by weak sr(p)-process. • 70Zn is strongly produced by SNII. It has a strong explosive component and secondary-like production factors (ww95).

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