WLW mass model in nuclear r-process calculations

Li Zhu; Niu Zhong-Ming; Sun Bao-Hua; Wang Ning; Meng Jie

doi:10.7498/aps.61.072601

Abstract

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:

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.

References

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[15]	Sun B, Meng J 2008 Chin. Phys. Lett. 25 2429
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Cited By

[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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Vol. 61, Issue 7 - 2012-04-05

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