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Chinese Physics C> 2016, Vol. 40> Issue(12) : 125101 DOI: 10.1088/1674-1137/40/12/125101

Reevaluation of thermonuclear reaction rate of 50Fe(p, γ)51Co

  • 1.

      College of Physics and Electronic Information Engineering, Chifeng University, Chifeng 024000, China

  • 2.

      Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China

  • 3.

      Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China

  • The thermonuclear rate of the 50Fe(p, γ)51Co reaction in the Type I X-ray bursts (XRBs) temperature range has been reevaluated based on a recent precise mass measurement at CSRe Lanzhou, where the proton separation energy Sp=142±77 keV has been determined firstly for the 51Co nucleus. Comparing to the previous theoretical predictions, the experimental Sp value has much smaller uncertainty. Based on the nuclear shell model and mirror nuclear structure information, we have calculated two sets of thermonuclear rates for the 50Fe(p, γ)51Co reaction by utilizing the experimental Sp value. It shows that the statistical-model calculations are not ideally applicable for this reaction primarily because of the low density of low-lying excited states in 51Co. In this work, we recommend that a set of new reaction rates based on the mirror structure of 51Cr should be incorporated in future astrophysical network calculations.
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  • References

    [1] S.E. Woosley and R.E. Taam, Nature, 263:101-103(1976)
    [2] P.C. Joss, Nature, 270:310-314(1977)
    [3] H. Schatz et al, Phys. Rev. Lett., 86:3471-3474(2001)
    [4] V.-V. Elomaa et al, Phys. Rev. Lett., 102:252501(2009)
    [5] R.K. Wallace and S.E. Woosley, Astrophys. J. Suppl., 45:389-420(1981)
    [6] H. Schatz et al, Phys. Rep., 294:167-263(1998)
    [7] S.E. Woosley et al, Astrophys. J. Suppl., 151:75-102(2004)
    [8] W. Lewin et al, Space Sci. Rev., 62:223-389(1993)
    [9] T. Strohmayer, L. Bildsten, in Compact Stellar X-Ray Sources, edited by W. Lewin and M. van der Klis (Cambridge:Cambridge Univ. Press, 2006)
    [10] A. Parikh et al, Prog. Part. Nucl. Phys., 69:225-253(2013)
    [11] A. Parikh et al, Phys. Rev. C, 79:045802(2009)
    [12] H. Schatz and K. E. Rehm, Nucl. Phys. A, 777:601-622(2006)
    [13] J. W. Xia et al, Nucl. Instrum. Methods A, 488:11-25(2002)
    [14] P. Shuai et al, Phys. Lett. B, 735:327-331(2014)
    [15] A.H. Wapstra and G. Audi, Nucl. Phys. A, 432:1-54(1985)
    [16] G. Audi and A.H. Wapstra, Nucl. Phys. A, 565:1-65(1993)
    [17] G. Audi and A.H. Wapstra, Nucl. Phys. A, 595:409-480(1995)
    [18] G. Audi, A.H. Wapstra, and C. Thibault, Nucl. Phys. A, 729:337-676(2003)
    [19] J.J. He et al, Phys. Rev. C, 89:035802(2014)
    [20] L. Van Wormer et al, Astrophy. J, 432:326-350(1994)
    [21] T. Rauscher and F.-K. Thielemann, At. Data Nucl. Data Tables, 75:1-351(2000)
    [22] T. Rauscher and F.-K. Thielemann, in Stellar Evolution, Stellar Explosions and Galactic Chemical Evolution, edited by A. Mezzacappa (IOP:Bristol, 1998)
    [23] P. Mller et al, At. Data Nucl. Data Tables, 59:185-381(1995)
    [24] J.M. Pearson et al, Phys. Lett. B, 387:455-459(1996)
    [25] J.L. Fisker et al, At. Data Nucl. Data Tables, 79:241-292(2001)
    [26] R.H. Cyburt et al, Astrophys. J. Suppl., 189:240-252(2010)
    [27] C.E. Rolfs and W.S. Rodney, Cauldrons in the Cosmos (Chicago:Univ. of Chicago Press, 1988)
    [28] J. Jos et al, Astrophys. J. Suppl., 189:204-239(2010)
    [29] A.R. Barnett et al, Comput. Phys. Commun., 8:377-395(1974)
    [30] X.L. Huang, Nucl. Data Sheets, 107:2131-2322(2006)
    [31] J.E. Robertshaw et al, Phys. Rev., 170:1013-1033(1968)
    [32] A.E. Macgregor and G. Brwon, Nucl. Phys. A, 190:548-564(1972)
    [33] M.S. Chowdhury, A.R. Majumder, and H.M. Sen Gupta, Nucl. Phys. A, 282:87-108(1977)
    [34] Z.D. Wu et al, Phys. Rev. C, 89:054315(2014)
    [35] C.A. Bertulani, Comput. Phys. Commun., 156:123-141(2003)
    [36] J.T. Huang, C.A. Bertulani, and V. Guimares, At. Data Nucl. Data Tables, 96:824-847(2010)

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Li-Ping Zhang, Jian-Jun He, Wan-Dong Chai, Su-Qing Hou and Li-Yong Zhang. Reevaluation of thermonuclear reaction rate of 50Fe(p, γ)51Co[J]. Chinese Physics C, 2016, 40(12): 125101. doi: 10.1088/1674-1137/40/12/125101
Li-Ping Zhang, Jian-Jun He, Wan-Dong Chai, Su-Qing Hou and Li-Yong Zhang. Reevaluation of thermonuclear reaction rate of 50Fe(p, γ)51Co[J]. Chinese Physics C, 2016, 40(12): 125101.  doi: 10.1088/1674-1137/40/12/125101 shu
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Received: 2016-07-25
Revised: 2016-09-19
Fund

    Supported by Natural Science Foundation of Inner Mongolia Autonomous Region of China (2013MS0916) and National Natural Science Foundation of China (11490562, 11405228)

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Reevaluation of thermonuclear reaction rate of 50Fe(p, γ)51Co

    Corresponding author: Jian-Jun He, hejianjun@nao.cas.cn
  • 1.  College of Physics and Electronic Information Engineering, Chifeng University, Chifeng 024000, China
  • 2.  Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
  • 3.  Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
  • Received Date: 2016-07-25
  • Accepted Date: 2016-09-19
  • Available Online: 2016-12-05
Fund Project:  Supported by Natural Science Foundation of Inner Mongolia Autonomous Region of China (2013MS0916) and National Natural Science Foundation of China (11490562, 11405228)

Abstract: The thermonuclear rate of the 50Fe(p, γ)51Co reaction in the Type I X-ray bursts (XRBs) temperature range has been reevaluated based on a recent precise mass measurement at CSRe Lanzhou, where the proton separation energy Sp=142±77 keV has been determined firstly for the 51Co nucleus. Comparing to the previous theoretical predictions, the experimental Sp value has much smaller uncertainty. Based on the nuclear shell model and mirror nuclear structure information, we have calculated two sets of thermonuclear rates for the 50Fe(p, γ)51Co reaction by utilizing the experimental Sp value. It shows that the statistical-model calculations are not ideally applicable for this reaction primarily because of the low density of low-lying excited states in 51Co. In this work, we recommend that a set of new reaction rates based on the mirror structure of 51Cr should be incorporated in future astrophysical network calculations.

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