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Sara Bisterzo (1)

s-Process in low metallicity Pb stars: comparison between new theoretical results and spectroscopic observations. Sara Bisterzo (1) Roberto Gallino (1) , Oscar Straniero (2) , I. I. Ivans (3, 4) , F. Käppeler (5) and Wako Aoki, Sean Ryan, Timoty C. Beers

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Sara Bisterzo (1)

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  1. s-Process in low metallicity Pb stars: comparison between new theoretical results and spectroscopic observations Sara Bisterzo (1) Roberto Gallino (1), Oscar Straniero (2), I. I. Ivans (3, 4),F. Käppeler (5) and Wako Aoki, Sean Ryan, Timoty C. Beers (1) Dipartimento di Fisica Generale , Università di Torino, 10125 (To) Italy (2) Osservatorio Astronomico di Collurania – Teramo, 64100 (3)The Observatories of the Carnegie Institution of Washington, Pasadena, CA, (USA) (4)Princeton University Observatory, Princeton, NJ (USA) (5)Forschungszentrum Karlsruhe, Institut für Kernphysik, D-76021 Karlsruhe, Germany VIII Torino Workshop, Granada, 6 – 11 Febr. 2006

  2. Outline: • Lead stars (C, s, Pb rich) • C and s+r rich Lead stars • s-enhanced stars and Pb predictions • Nb: indicator of an extrinsic AGB in a binary system • Na (and Mg): permits an estimate of the initial AGB stellar mass.

  3. 1.2 Msun  3 pulses 1.3 Msun  6 pulses 1.4 Msun  8 pulses 1.5 Msun  20 pulses 2 Msun  26 pulses 3 Msun  30 pulses AGB models at very low [Fe/H] 1.2 Msun < M < 3 Msun M = 1.5 Msun 13C-pocket: ST*2 …. ST/100 Constant pulse by pulse (ST: 4.10-6 Msun , [Fe/H] = -0.3,Reproduction of Solar Main Component ) Mass loss : from 10-7 to 10-4 Msun/yr  Reimers 1.2 Msun  η = 0.3 1.3 Msun  η = 0.3 1.4 Msun  η = 0.3 1.5 Msun  η = 0.3 2 Msun  η = 0.5 3 Msun  η = 1

  4. Extrinsic AGB models Diluition factor: used to simulate the mixing effect in the envelope of the extrinsic stars Note: for main sequence stars dil ≈ 0  for giants dil may be important

  5. [ls/Fe] versus [Fe/H] ls = <Y, Zr> M = 1.5 MΘ M = 1.3 MΘ 3 3 2 2 1 1 M = 2 MΘ 3 3 2 2 M = 3 MΘ

  6. [hs/ls] versus [Fe/H] Example: ST/2 at [Fe/H] = -2 Example: ST/12 at [Fe/H] = -2.5 M = 1.3 MΘ M = 1.5 MΘ 1 1 0 0 M = 2 MΘ M = 3 MΘ 1 1 0 0 -1 -1

  7. [hs/ls] for different masses at [Fe/H] = -2.6  1 dex  1.5 dex

  8. [Pb/hs] versus [Fe/H]

  9. To reproduce stars with both s+r enhancements Different choice of initial chemical abundances of Eu in the progenitor clouds [Eu/Fe]ini from 0.5 to 1.5 and 2.0

  10. Effect of pre r-enrichment in s-enhanced stars AGB star model of M = 1.3 Msun with [Fe/H] = - 2.60. NO r-process rich r-process rich [Eu/Fe]ini = 0.0 [Eu/Fe]ini = 2.0 Model with pre r-enrichment normalized to [Eu/Fe]ini = 2.0 in the parental cloud: the envelope abundances in these stars are predicted by mass transfer from the more massive AGB companion in a binary system which formed from a parental cloud already enriched in r elements.

  11. Choice of initial abundances The choice of the initial r-rich isotope abundances normalised to Eu is made considering the r-process solar prediction from Arlandini et al.1999.

  12. 1- Lead stars (C, s, Pb rich)2 – C and s+r rich Lead stars

  13. 1. J. A. Johnson, M. Bolte, ApJ 579, L87 (2002) 2. W. Aoki, et al., ApJ 580, 1149 (2002) 3. T. Sivarani, et al., A&A 413, 1073 (2004) 4. J. A. Johnson, M. Bolte, ApJ 605, 462 (2004) 5. W. Aoki, et al., PASJ 54, 427 (2002) 6. S. Van Eck et al., A&A 404, 291 (2003) 7. S. Lucatello, et al., AJ 125, 875 (2003) 8. J. G. Cohen et al., ApJ 588, 1082 (2003) 9. B. Barbuy, et al., A&A 429, 1031 (2005) 10. I. Ivans et al., ApJ 627, 145 (2005) 11. K. Jonsell et al., astroph 1476J (2006)

  14. CS 22880-074 Aoki et al. 2002 Teff = 5850

  15. HE 0024-2543 Lucatello et al. 2003 Teff = 6625

  16. 2 – C and s+r rich Lead stars

  17. HE2148-1247 Cohen et al. 2003 M ≈ 1.3 Msun M ≈ 1.3 Msun 0.0 With r-process enhancement  [Eu/Fe] ini = 2.0 Without r-process enhancement  [Eu/Fe] ini = 0.0 Teff = 6380 K

  18. Jonsell et al. 2006 astroph With r-process enhancement  [Eu/Fe] ini = 2.0 Teff = 6160

  19. CS29497-34 Barbuy et al. 2005 With r-process enhancement  [Eu/Fe] ini = 1.5 Teff = 4800

  20. CS31062-050 Aoki et al. 2002 With r-process enhancement  [Eu/Fe] ini = 1.8 Teff = 5600

  21. Barklem et al. 2005: s-enhanced stars ** Pb predictions 12. Barklem et al., A&A 439, 129 (2005)

  22. HE 1105+0027 Barklem et al. 2005 With r-process enhancement  [Eu/Fe] ini = 1.8 Teff = 6132 Pb prediction  3

  23. HE 2150-0825 Barklem et al. 2005 Without r-process enhancement Teff = 5960 Pb prediction  3.5

  24. [Pb/Fe] versus [Fe/H]

  25. [Pb/hs] versus [Fe/H]

  26. Spectroscopic Na (and Mg)  Stellar Mass prediction AGB models of M = 1.3, 1.5, 3 Msun, for the same 13C-pocket, at [Fe/H] = – 2.60. A strong primary production of 22Ne results in advanced pulses, by conversion of primary 12C to 14N in the H-burning ashes, followed by 2a captures on 14N in the thermal pulses and implies a primary production of 23Na via 22Ne(n,g)23Na, (and 23Na(n,g)24Na(b-)24Mg).

  27. Zr over Nb: Intrinsic or Extrinsic AGBs s-process path The s elements enhancement in low-metallicity stars interpreted by mass transfer in binary systems (extrinsic AGBs). For extrinsic AGBs [Zr/Nb] ~ 0. Instead, for intrinsic AGBs [Zr/Nb] ~ 1.

  28. CONCLUSIONS: The spectroscopic abundances of low-metallicity s- and r-process enriched stars are interpreted using theoretical AGB models (FRANEC CODE),with an initial composition already enriched in r elements from the parental cloud from which the binary system was formed. • [Zr/Nb] is an indicator of an extrinsic AGB in a binary system: [Zr/Nb] ~ 0 for an extrinsic AGB, [Zr/Nb] ~ – 1 for an intrinsic AGB. • Spectroscopic determination of [Na/Fe] and [Mg/Fe] permits an estimate of the initial AGB stellar mass.

  29. CONCLUSIONS: • Open Problem: the strong discrepancy of C and N predictions with respect to observations may be reconciled: • by introducing the effect of cool bottom process (CBP) in the TP-AGB phase (*); • for N and [Fe/H] < -2.3, by the effect of Huge First TDU. • Uncertainties in the spectroscopic abundances of C, N, O, Na, Mg  M. Asplund, ARAA 2005 (*) Nollett, K. M., Busso, M., Wasserburg, G. J., ApJ 582, 1036 (2003); Wasserburg, G. J., Busso, M., Gallino, R., Nollett, K. M., (2006), Nucl. Physics, in press.

  30. [hs/Fe] versus [Fe/H] hs = <Ba, La, Nd, Sm> M = 1.5 MΘ M = 1.3 MΘ 3 3 2 2 1 1 M = 2 MΘ M = 3 MΘ 3 3 2 2 1 1

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