Chinese Physics C > 2003, Vol. 27 > Issue(4): 304-308

Abundances of Metal-Poor Stars and Slow Neutron-Capture Progress

Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039, China2 Department of Physics and Eletronic Science, Guangxi Normal University, Guilin 541004, China3 Department of Physics, Hebei Normal University, Shijiazhuang 050016, China4 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator of Lanzhou, Lanzhou 730000, China

Abstract
HTML
Reference
Related

PDF

Abstract：
We apply the parametric model to fit the surface abundances of three lead rich stars (HD187861, HD196944 and HD224959) without adopting any specific stellar model. It shows that the calculated result can fit the observed data well whether the reaction branchings are taken into account or not. Besides, by the comparison of the model parameters of the three lead rich stars with those of two very metal poor stars (LP625 44 and LP706 7), we find out that the average neutron exposure of the former is larger than that of the latter, but the dredge up extent is smaller. We come to the conclusion that the parametric model is significant of constraints on the stellar model, though it is very simple.

References

[1]

. Burbidge E M ,Berbidge G R ,Fowler W A et al.Rev.Mod.Phys.,1957,29:547—6502. LI GuangLie,LI Long.Nuclear Physics Review,1999,16:201—206(in Chinese)(厉光烈,李龙.原子核物理评论,1999,16:201—206)3. ZHANG MiaoJing,ZHANG Bo,LI GuangLie.Nuclear Physics Review,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)4. Gallino R ,Arlandini C ,Busso M et al.Ap.J.,1998,497:388—4035. Van Eck S ,Goriely S ,Jorissen A et al.Nature,2001,412:793—7956. Aoki W ,Ryan S G ,Norris J E et al.Ap.J .,2001,561:346—3637. Howard W M ,Mathews G J, Takahashi K et al. Ap.J.,1986,309:633—6528. Arlandini C , K ppeler F ,Wisshak K et al. Ap.J .,1999,525:886—9009. BAO Z Y ,Beer H ,K ppeler F et al.Atomic Data and Nuclear Data Tables,2000,76:70—154

[1]	ZHANG Yu-Mei,XU Fu-Rong. β-Decay of Neutron-Rich Nucleus¹⁸N. Chinese Physics C, 2006, 30(S2): 115-117.
[2]	WEN Hai-Bao. Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars. Chinese Physics C, 2005, 29(7): 657-663.
[3]	MA Yu-Gang,WEI Yi-Bin,SHEN Wen-Qing,CAI Xiang-Zhou,CHEN Jin-Gen,FANG De-Qing,GUO Wei,MA Guo-Liang,SU Qian-Min,TIAN Wen-Dong,WANG Kun,ZHONG Chen,ZHOU Xing-Fei. HBT Study of Reactions Induced by Neutron-Rich Nuclei at Intermediate Energy. Chinese Physics C, 2004, 28(S1): 16-20.
[4]	SHEN Gang,MENG Jie,Hillhouse G. Direct URCA Process in Neutron Stars. Chinese Physics C, 2004, 28(S1): 99-101.
[5]	ZHANG Miao-Jing,ZHANG Bo,LI Guang-Lie. Neutron Capture Elements in Poor-Metal Stars. Chinese Physics C, 2004, 28(1): 30-36.
[6]	GUO Hua,LIU Bo,LI Xi-Guo,CHEN Yan-Jun. Kaon Condensation in Neutron Star Matter. Chinese Physics C, 2003, 27(2): 113-117.
[7]	Soojae Im,LI Zeng-Hua. Properties of the Neutron Mean Potential in the Neutron-Rich Nuclei. Chinese Physics C, 2003, 27(6): 507-510.
[8]	ZHANG Miao-Jing,ZHANG Bo,LI Guang-Lie. Abundance Distribution in the Solar System and Slow Neutron Capture Elements in AGB Stars. Chinese Physics C, 2003, 27(11): 978-983.
[9]	LIU Jian-Feng,ZHAO Wei-Juan. Stuty on the Process of the Fast Neutron Radiative Capture for⁴⁰Ca and²⁰⁸Pb. Chinese Physics C, 2002, 26(11): 1158-1165.
[10]	LIU Jian-Feng,ZHAO Wei-Juan,WANG Feng-Ge,SU Zong-Di. Study on γ-Ray Strength Functions and Energy Spectra in the Neutron Radiative Capture of¹⁹⁷Au. Chinese Physics C, 2001, 25(10): 994-1001.
[11]	LI Wen-Fei,ZHANG Feng-Shou,CHEN Lie-Wen. On the Moment of Inertia and Surface Redshift of Neutron Star. Chinese Physics C, 2001, 25(10): 1006-1011.
[12]	SUN Bao-Xi,JIA Huan-Yu,MENG Jie,ZHAO En-Guang. Neutron Star in Relativistic Mean-field Approximation. Chinese Physics C, 2000, 24(S1): 69-72.
[13]	Lu Minghui,Ma Weixing,Bijan Saghai,Li Zhenping. Study of K-meson Photoproduction and Associated Radiative Capture Process. Chinese Physics C, 1998, 22(3): 255-259.
[14]	Zhang Changhua,Gu Jinnan. Shell Model Calculations for Light Neutron-Rich Nuclei. Chinese Physics C, 1996, 20(3): 240-245.
[15]	ZHU Sheng-Jiang. Research on Level Structures of Neutron-Rich Nuclei and Shape Phase Transitions Around A～100 and 150 Regions. Chinese Physics C, 1993, 17(4): 353-361.
[16]	MU Yun-Shan,XU Hai-Shan,XIANG Zheng-Yu,LI Ye-Xiang,WANG Shi-Ming,LIU Jian-Feng. Fast Neutron Capture Cross Section of Natural Molybdenum. Chinese Physics C, 1991, 15(1): 66-70.
[17]	XIANG Zheng-Yu,XU Hai-Shan,LI Ye-Xiang,MU Yun-Shan,WANG Shi-Ming,LIU Jian-Feng. FAST NEUTRON CAPTURE CROSS SECTIONS OF FISSION PRODUCT NUCLIDE Eu. Chinese Physics C, 1989, 13(10): 938-941.
[18]	WANG Bing,SHEN Wen-Qing,FENG Jun,ZHU Yong-Tai,FENG En-Pu. THE NEUTRON EXCESS DEPENDENCE OF TOTAL REACTION CROSS SECTION IN THE INTERMEDIATE ENERGY DOMAIN. Chinese Physics C, 1989, 13(6): 553-559.
[19]	LIU Jian-Feng,HUO Yu-Kun. RADIATIVE CAPTURE IN THE INELASTIC CHANNEL OF THE COMPOUND NUCLEUS. Chinese Physics C, 1983, 7(3): 355-360.
[20]	HO YU-KUN. NEUTRON CAPTURE GAMMA RAY SPECTRA AT LOW ENERGY. Chinese Physics C, 1981, 5(6): 732-740.

Access

Get Citation

ZHANG Miao-Jing, ZHANG Bo, LIU Ji-Hong and LI Guang-Lie. Abundances of Metal-Poor Stars and Slow Neutron-Capture Progress[J]. Chinese Physics C, 2003, 27(4): 304-308.

ZHANG Miao-Jing, ZHANG Bo, LIU Ji-Hong and LI Guang-Lie. Abundances of Metal-Poor Stars and Slow Neutron-Capture Progress[J]. Chinese Physics C, 2003, 27(4): 304-308. shu

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2002-07-15
Revised: 1900-01-01

Article Metric

Article Views(2703)
PDF Downloads(550)
Cited by(0)

Policy on re-use

To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.

通讯作者:陈斌, bchen63@163.com

1.
沈阳化工大学材料科学与工程学院沈阳 110142

Abundances of Metal-Poor Stars and Slow Neutron-Capture Progress

Corresponding author:ZHANG Miao-Jing,

Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039, China2 Department of Physics and Eletronic Science, Guangxi Normal University, Guilin 541004, China3 Department of Physics, Hebei Normal University, Shijiazhuang 050016, China4 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator of Lanzhou, Lanzhou 730000, China

Received Date:2002-07-15
Accepted Date:1900-01-01
Available Online:2003-04-05

Abstract:We apply the parametric model to fit the surface abundances of three lead rich stars (HD187861, HD196944 and HD224959) without adopting any specific stellar model. It shows that the calculated result can fit the observed data well whether the reaction branchings are taken into account or not. Besides, by the comparison of the model parameters of the three lead rich stars with those of two very metal poor stars (LP625 44 and LP706 7), we find out that the average neutron exposure of the former is larger than that of the latter, but the dredge up extent is smaller. We come to the conclusion that the parametric model is significant of constraints on the stellar model, though it is very simple.