WLW 原子核质量模型在r过程研究中的应用

李竹; 牛中明; 孙保华; 王宁; 孟杰

doi:10.7498/aps.61.072601

摘要

本工作利用最近提出的WLW宏观-微观原子核质量模型, 在经典r过程框架下很好地描述了太阳系r过程核素丰度分布. 与常用的FRDM质量模型相比, 新计算更好地再现了A135和A180质量区的太阳系r过程核素丰度, 尤其避免了其他相似计算中A=135 附近出现的与观测不符的丰度峰问题. 分析表明, 这种差异可能暗示WLW更为合理地处理了壳结构和对称能.

关键词:

The rapid neutron-capture process (r-process), which is an interdisciplinary field of astrophysics and nuclear physics, is bound up with various characteristics of thousands of neutron-rich exotic nuclei, such as nuclear masses, and the relevant reactions. By employing the WLW microscopic-macroscopic nuclear mass model developed recently, the solar r-process abundance distribution is well reproduced in the classical r-process approach. In comparison with the well known FRDM model, the present calculation better pictures the nuclear region of A135 and A180, and especially avoids the abundance peaks at A135 often obtained in other calculations. The improvement in the r-process calculation may indicate a more suitable description of the evolution of shell structure and symmetry energy towards the drip line in the WLW model.

Keywords:

作者及机构信息

1.
北京航空航天大学物理科学与核能工程学院, 北京 100191;

2.
北京大学物理学院, 北京 100871;

3.
广西师范大学物理系, 桂林 541004

基金项目: 北航国家大学生科研训练计划(SRTP)项目基金, 新世纪优秀人才支持计划, 973项目(批准号: 2007CB815000)和国家自然科学基金(批准号: 10975007, 10975008, 11105010 和11128510)资助的课题.

Authors and contacts

1.
School of Physics Science and Nuclear Engineering, Beihang University, Beijing 100191, China;

2.
School of Physics, Peking University, Beijing 100871 China;

3.
Department of Physics, Guangxi Normal University, Gulin 541004, China

Funds: Project supported by the Major State 973 Program (Grant No. 2007CB815000), the National Natural Science Foundation of China (Grants Nos. 10975007, 10975008, 11105010 and 11128510), Beihang University SRTP and Program for New Century Excellent Talents in University.

参考文献

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[2]	Arnould M, Goriely S, Takahashi K 2007 Phys. Rep. 450 97
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[4]	Ning H, Qian Y Z, Meyer B S 2007 Astrophys. J. 667 L159
[5]	Freiburghaus C, Rosswog S, Thielemann F K 1999 Astrophys. J. 525 L121
[6]	Goriely S, Demetriou P, Janka H T, Pearson J M, Samyn M 2005 Astrophys. J. 758 587
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[8]	Pearson J M, Nayak R C, Goriely S 1996 Phys. Lett. B 387 455
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[12]	Sun B, Montes F, Geng L S, Geissel H, Litvinov Y A, Meng J 2008 Phys. Rev. C 78 025806
[13]	Wanajo S, Goriely S, Samyn M, Itoh N 2004 Astrophys. J. 606 1057
[14]	Pfeiffer B, Kratz K L, Thielemann F K 1997 Z. Phys. A 357 235
[15]	Sun B, Meng J 2008 Chin. Phys. Lett. 25 2429
[16]	Niu Z M, Sun B, Meng J 2009 Phys. Rev. C 80 065806
[17]	Fu G J, Zhao Y M, Pittel S, Arima A 2010 Phys. Rev. C 82 034304
[18]	Sun B, Zhao P W, Meng J 2011 Science China G 54 210
[19]	Wang N, Liu M, Wu X 2010 Phys. Rev. C 81 044322
[20]	Wang N, Liang Z, Liu M, Wu X 2011 Phys. Rev. C 82 044304
[21]	Audi G, Bersillon O, Blachot J, Wapstra A H 2003 Nucl. Phys. A 729 3
[22]	Kratz K L, Bitouzet J P, Thielemann F K,Moller P, Pfeiffer B 1993 Astrophys. J. 403 216
[23]	Kratz K L, Farouqi K, Pfeiffer B, Truran J W, Sneden C, Cowan J J 2007 Astrophys. J. 662 39
[24]	Chen B, Dobaczewski J, Kratz K L, Langanke K, Pfeiffer B, Thielemann F K, Vogel P 1995 Phys. Lett. B 355 37
[25]	Simmerer J, Sneden C, Cowan J J, Collier J, Woolf V M, Lawler J E 2004 Astrophys. J. 617 1091
[26]	Möller P, Pfeiffer B, Kratz K L 2003 Phys. Rev. C 67 055802

施引文献

[1]	Burbidge E M, Burbidge G R, Fowler W A, Hoyle F 1957 Rev. Mod. Phys. 29 547
[2]	Arnould M, Goriely S, Takahashi K 2007 Phys. Rep. 450 97
[3]	Cameron A G W 2001 Astrophys. J. 562 456
[4]	Ning H, Qian Y Z, Meyer B S 2007 Astrophys. J. 667 L159
[5]	Freiburghaus C, Rosswog S, Thielemann F K 1999 Astrophys. J. 525 L121
[6]	Goriely S, Demetriou P, Janka H T, Pearson J M, Samyn M 2005 Astrophys. J. 758 587
[7]	Möller P, Nix J R, Myers W D, Swiatecki W J 1995 Atomic Data and Nuclear Data Tables 59 185
[8]	Pearson J M, Nayak R C, Goriely S 1996 Phys. Lett. B 387 455
[9]	Goriely S, Samyn M, Heenen P H, Pearson J M, Tondeur F 2002 Phys. Rev. C 66 024326
[10]	Geng L S, Toki H, Meng J 2005 Prog. Theor. Phys. 113 785
[11]	Sun B, Knöbel R, Litvinov Y A, Geissel H, Meng J, Beckert K, Bosch F, Boutin D, Brandau C, Chen L, Cullen I J, Dimopoulou C, Fabian B, Hausmann M, Kozhuharov C, Litvinov S A, Mazzocco M, Montes F, Müzenberg G, Musumarra A, Nakajima S, Nociforo C, Nolden F, Ohtsubo T, Ozawa A, Patyk Z, Plaß W R, Scheidenberger C, Steck M, Suzuki T, Walker P M, Weick H, Winckler N, Winkler M, Yamaguchi T 2008 Nucl. Phys. A 812 1
[12]	Sun B, Montes F, Geng L S, Geissel H, Litvinov Y A, Meng J 2008 Phys. Rev. C 78 025806
[13]	Wanajo S, Goriely S, Samyn M, Itoh N 2004 Astrophys. J. 606 1057
[14]	Pfeiffer B, Kratz K L, Thielemann F K 1997 Z. Phys. A 357 235
[15]	Sun B, Meng J 2008 Chin. Phys. Lett. 25 2429
[16]	Niu Z M, Sun B, Meng J 2009 Phys. Rev. C 80 065806
[17]	Fu G J, Zhao Y M, Pittel S, Arima A 2010 Phys. Rev. C 82 034304
[18]	Sun B, Zhao P W, Meng J 2011 Science China G 54 210
[19]	Wang N, Liu M, Wu X 2010 Phys. Rev. C 81 044322
[20]	Wang N, Liang Z, Liu M, Wu X 2011 Phys. Rev. C 82 044304
[21]	Audi G, Bersillon O, Blachot J, Wapstra A H 2003 Nucl. Phys. A 729 3
[22]	Kratz K L, Bitouzet J P, Thielemann F K,Moller P, Pfeiffer B 1993 Astrophys. J. 403 216
[23]	Kratz K L, Farouqi K, Pfeiffer B, Truran J W, Sneden C, Cowan J J 2007 Astrophys. J. 662 39
[24]	Chen B, Dobaczewski J, Kratz K L, Langanke K, Pfeiffer B, Thielemann F K, Vogel P 1995 Phys. Lett. B 355 37
[25]	Simmerer J, Sneden C, Cowan J J, Collier J, Woolf V M, Lawler J E 2004 Astrophys. J. 617 1091
[26]	Möller P, Pfeiffer B, Kratz K L 2003 Phys. Rev. C 67 055802

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