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Chinese Physics C> 2003, Vol. 27> Issue(11) : 978-983 

Abundance Distribution in the Solar System and Slow Neutron Capture Elements in AGB Stars

  •  Academy of Physics and Information Engineering, Guangxi Normal University, Guilin 541004, China2 Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039, China3 Department of Physics, Hehei Normal University, Shijiazhuang 050016, China4 Center of Theoretical Nuclear Physics, National laboratory of Heavy Ion Accelerator of Lanzhou, I-an/.hou 730000, China

  • By re-analyzing the results of the theoretical abundance of AGB stellar models and the observed abundances of 51 AGB samples, we find that the abundance distribution of heavy elements belonging to the main-component of slow neutron capture process (SMH elements) of any AGB star is similar to that of the scaled s-process main component of the solar system. It means that superposition of the SMH element abundance distributions of AGB stars should be similar to that of the scaled solar s-main component. As a conclusion, the heavy element abundance pattern of the solar s-main component is a typical one and can be used as a standard in the investigation of heavy element abundances in single star.
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    [1] Burbidge E M, Berbidge G R, Fowler W A et al. Rev. Mod. Phys., 1957,29: 547–6502 ZHANG Miao–Jing, ZHANG Bo, LI Guang–Lie. Nucl. Phys. Rev., 2002,19:321–328(in Chinese)(张妙静,张波,厉光烈.原子核物理评论,2002,19:321–328)3 Wallerstein G, Greenstein J L, Parker R et al. Ap. J., 1963,137:280–3004 Spite M, Spite F. Astron, Astrophys., 1978,67:23–315 Woolf V M, Tomkin J, Lambert D L. Ap. J., 1995,453:660–6726 Gallino R, Arlandini C, Busso M et al. Ap. J., 1998,497:388–4037 Travaglio C, Galli D, Gallino R et al. Ap. J., 1999,521:691–7028 Busso M, Gallino R,Lambert D Let al. Ap. J., 2001,557:802–8219 Arlandini C, Kppeler F, Wisshak K et al. Ap. J., 1999,525:886–90010 Luck R E, Bond H E. Ap. J., 1985, 292:559–57711 Luck R E, Bond H E. Ap. J. Suppl., 1991,77:515–54012 Abia C, Wallerstein G. Mon. Not. R. Astron. Soc., 1998,293:89–10613 Abia C, Isern J. Ap. J., 2000,536:438–449 14 Abia C, Dominguez I, Gallino R et al. Ap. J., 2002,579:817–83115 Van Eck S, Goriely S, Jorissen A et al. Nature, 2001,412:793–79516 Aoki Wako, Ryan S G, Norris J E et al. Ap. J., 2001,561:346–36317 ZHANG Miao–Jing et al. High Energy Phys. and Nucl. Phys., 2003, 27(4) :304–308(in Chinese)(张妙静等.高能物理与核物理,2003,27(4) :304–308)

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ZHANG Miao-Jing, ZHANG Bo and LI Guang-Lie. Abundance Distribution in the Solar System and Slow Neutron Capture Elements in AGB Stars[J]. Chinese Physics C, 2003, 27(11): 978-983.
ZHANG Miao-Jing, ZHANG Bo and LI Guang-Lie. Abundance Distribution in the Solar System and Slow Neutron Capture Elements in AGB Stars[J]. Chinese Physics C, 2003, 27(11): 978-983. shu
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Received: 2003-04-29
Revised: 1900-01-01
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Abundance Distribution in the Solar System and Slow Neutron Capture Elements in AGB Stars

    Corresponding author: ZHANG Miao-Jing,
  • Academy of Physics and Information Engineering, Guangxi Normal University, Guilin 541004, China2 Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039, China3 Department of Physics, Hehei Normal University, Shijiazhuang 050016, China4 Center of Theoretical Nuclear Physics, National laboratory of Heavy Ion Accelerator of Lanzhou, I-an/.hou 730000, China
  • Received Date: 2003-04-29
  • Accepted Date: 1900-01-01
  • Available Online: 2003-11-05

Abstract: By re-analyzing the results of the theoretical abundance of AGB stellar models and the observed abundances of 51 AGB samples, we find that the abundance distribution of heavy elements belonging to the main-component of slow neutron capture process (SMH elements) of any AGB star is similar to that of the scaled s-process main component of the solar system. It means that superposition of the SMH element abundance distributions of AGB stars should be similar to that of the scaled solar s-main component. As a conclusion, the heavy element abundance pattern of the solar s-main component is a typical one and can be used as a standard in the investigation of heavy element abundances in single star.

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