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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2018, Vol. 42> Issue(6) : 064105 DOI: 10.1088/1674-1137/42/6/064105

The symmetry energy γ parameter of relativistic mean-field models

  • 1.

      Departamento de Ciê

  • 2.

      Universidade Federal do Rio de Janeiro, 27930-560, Macaé

  • 3.

      Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA

  • 4.

      School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel

  • 5.

      Depto de Fí

  • The relativistic mean-field models tested in previous works against nuclear matter experimental values, critical parameters and macroscopic stellar properties are revisited and used in the evaluation of the symmetry energy γ parameter obtained in three different ways. We have checked that, independent of the choice made to calculate the γ values, a trend of linear correlation is observed between γ and the symmetry energy (S0) and a more clear linear relationship is established between γ and the slope of the symmetry energy (L0). These results directly contribute to the arising of other linear correlations between γ and the neutron star radii of R1.0 and R1.4, in agreement with recent findings. Finally, we have found that short-range correlations induce two specific parametrizations, namely, IU-FSU and DD-MEδ, simultaneously compatible with the neutron star mass constraint of 1.93≤Mmax/M⊙≤2.05 and with the overlap band for the L0×S0 region, to present γ in the range of γ=0.25±0.05.
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    [1] M. Dutra, O. Lourenco, S. S. Avancini, B. V. Carlson, A. Delfino, D. P. Menezes, C. Providencia, S. Typel, and J. R. Stone, Phys. Rev. C, 90:055203 (2014)
    [2] M. Dutra, O. Lourenco, and D. P. Menezes, Phys. Rev. C, 93:025806 (2016); Phys. Rev. C, 94:049901(E) (2016)
    [3] P. B. Demorest, T. Pennucci, S. M. Ransom, M. S. E. Roberts, and J. W. T. Hessels, Nature, 467:1081 (2010)
    [4] J. Antoniadis, P. C. C. Freire, N. Wex et al, Science, 340:448 (2013)
    [5] O. Lourenco, M. Dutra, and D. P. Menezes, Phys. Rev. C, 95:065212 (2017)
    [6] G. Bertsch and P. J. Siemens, Phys. Lett. B, 126:9 (1983); J. Margueron and P. Chomaz, Phys. Rev. C, 67:041602 (2003); C. Ducoin, Ph. Chomaz, and F. Gulminelli, Nucl. Phys. A, 771:68 (2006)
    [7] H. Mller and B. D. Serot, Phys. Rev. C, 52:2072 (1995)
    [8] Ph. Chomaz, C. Colonna, and J. Randrup, Phys. Rep., 389:263 (2004)
    [9] J. B. Silva, O. Lourenco, A. Delfino, J. S. Sa Martins, and M. Dutra, Phys. Lett. B, 664 246, (2008)
    [10] V. Vovchenko, D. V. Anchishkin, and M. I. Gorenstein, Phys. Rev. C, 91:064314 (2015)
    [11] V. Vovchenko, D. V. Anchishkin, M. I. Gorenstein, and R. V. Poberezhnyuk, Phys. Rev. C, 92:054901 (2015)
    [12] V. Vovchenko, Phys. Rev. C, 96:015206 (2017)
    [13] M. Baldo, G. F. Burgio, Prog. Part. Nucl. Phys., 91:203 (2016)
    [14] C. J. Horowitz and J. Piekarewicz, Phys. Rev. Lett., 86:5647 (2001)
    [15] S. S. Avancini, J. R. Marinelli, D. P. Menezes, M. M. W. Moraes, and C. Providencia, Phys. Rev. C, 75:055805 (2007)
    [16] L. L. Lopes and D. P. Menezes, Braz. Jour. Phys., 44:774 (2014)
    [17] R. Cavagnoli, D. P. Menezes, and C. Providencia, Phys. Rev. C, 84:065810 (2011)
    [18] P. K. Panda, A. M. S. Santos, D. P. Menezes, and C. Providencia, Phys. Rev. C, 85:055802 (2012)
    [19] C. Providencia et al, Eur. Phys. J. A, 50:44 (2014)
    [20] H. Pais, A. Sulaksono, B. K. Agrawal, and C. Providencia, Phys. Rev. C, 93:045802 (2016)
    [21] S. S. Avancini, L. Brito, J. R. Marinelli, D. P. Menezes, M. M. W. de Moraes, C. Providencia, and A. M. Santos, Phys. Rev. C, 79:035804 (2009)
    [22] M. B. Tsang, Yingxun Zhang, P. Danielewicz, M. Famiano, Zhuxia Li, W. G. Lynch, and A. W. Steiner, Phys. Rev. Lett., 102:122701 (2009)
    [23] Andrew W. Steiner, James M. Lattimer, and Edward F. Brown, Astrophys J., 722:33 (2010)
    [24] Or Hen, Bao-An Li, Wen-Jun Guo, L. B. Weinstein, and Eliezer Piasetzky, Phys. Rev. C, 91:025803 (2015)
    [25] P. Russotto et al, Phys. Rev. C, 94:034608 (2016)
    [26] J. Meng, H. Toki, S. G. Zhou, S. Q. Zhang, W. H. Long, and L. S. Geng, Prog. Part. Nucl. Phys., 57:470 (2006)
    [27] B. K. Agrawal, Phys. Rev. C, 81:034323 (2010)
    [28] S. K. Dhiman, R. Kumar, and B. K. Agrawal, Phys. Rev. C, 76:045801 (2007)
    [29] B.-J. Cai and L.-W. Chen, Phys. Rev. C, 85:024302 (2012)
    [30] B. G. Todd-Rutel and J. Piekarewicz, Phys. Rev. Lett., 95:122501 (2005)
    [31] J. Piekarewicz and S. P. Weppner, Nucl. Phys. A, 778:10 (2006)
    [32] R. Kumar, B. K. Agrawal, and S. K. Dhiman, Phys. Rev. C, 74:034323 (2006)
    [33] A. Sulaksono and T. Mart, Phys. Rev. C, 74:045806 (2006)
    [34] F. J. Fattoyev, C. J. Horowitz, J. Piekarewicz, and G. Shen, Phys. Rev. C, 82:055803 (2010)
    [35] C. J. Horowitz and J. Piekarewicz, Phys. Rev. C, 66:055803 (2002)
    [36] T. Klahn et al, Phys. Rev. C, 74:035802 (2006)
    [37] S. Typel and H. H. Wolter, Nucl. Phys. A, 656:331 (1999)
    [38] T. Gaitanos, M. Di Toro, S. Typel, V. Baran, C. Fuchs, V. Greco, and H. H. Wolter, Nucl. Phys. A, 732:24 (2004)
    [39] X. Roca-Maza, X. Vinas, M. Centelles, P. Ring, and P. Schuck, Phys. Rev. C, 84:054309 (2011)
    [40] J. J. Rusnak and R. J. Furnstahl, Nucl. Phys. A, 627:495 (1997)
    [41] B. A. Nikolaus, T. Hoch, and D. G. Madland, Phys. Rev. C, 46:1757 (1992)
    [42] D. G Madland, T. J Brvenich, J. A Maruhn, and P.-G Reinhard, Nucl. Phys. A 741:52 (2004)
    [43] O. Lourenco, M. Dutra, A. Delfino, and R. L. P. G. Amaral, Int. Jour. Mod. Phys. E, 16:3037 (2007)
    [44] T. Niksic, D. Vretenar, and P. Ring, Prog. in Part. and Nucl. Phys., 66:519 (2011)
    [45] R. Subedi et al, Science, 320:1476 (2008)
    [46] O. Hen et al, Science, 346:614 (2014)
    [47] O. Hen, G. A. Miller, E. Piasetzky, and L. B. Weinstein, to apear in Rev. Mod. Phys., (2017)
    [48] J. M. Lattimer and Y. Lim, Astrophys. J., 51:771 (2013)
    [49] Neutron Star Crust:editors Carlos Bertulani and Jorge Pieckarewicz, Nova Science Publishers, 2012, New York
    [50] B. M. Santos, M. Dutra, O. Lourenco, and A. Delfino, Phys. Rev. C, 90:035203 (2014); 92:015210 (2015)
    [51] S. Brandt, Data Analysis:Statistical and Computational Methods for Scientists and Engineers:4th ed. (Springer, New York, 2014)
    [52] N. Alam, B. K. Agrawal, M. Fortin, H. Pais, C. Providencia, Ad. R. Raduta, and A. Sulaksono, Phys. Rev. C, 94:052801(R) (2016)
    [53] G. Baym, C. Pethick, and P. Sutherland, Astrophys. J., 170:299 (1971)
    [54] J. R. Oppenheimer, G. M. Volkoff, Phys. Rev., 33:374 (1939)
    [55] N. K. Glendenning, Compact Stars:2nd ed. (Springer, New York, 2000); P. Haensel, A. Y. Potekhin, and D. G. Yakovlev, Neutron Stars, Equation of State and Structure (Springer, New York, 2006)
    [56] Bao-An Li, W. Udo Schrder (Eds.), Isospin Physics in Heavy-Ion Collisions at Intermediate Energies:Nova Science Publishers, Huntington, NY, 2001
    [57] Bao-An Li, Champak B. Das, Subal Das Gupta, and Charles Gale, Nuc. Phys. A, 735:563 (2004)

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Mariana Dutra, Odilon Louren, Or Hen, Eliezer Piasetzky and Débora P. Menezes. The symmetry energy γ parameter of relativistic mean-field models[J]. Chinese Physics C, 2018, 42(6): 064105. doi: 10.1088/1674-1137/42/6/064105
Mariana Dutra, Odilon Louren, Or Hen, Eliezer Piasetzky and Débora P. Menezes. The symmetry energy γ parameter of relativistic mean-field models[J]. Chinese Physics C, 2018, 42(6): 064105.  doi: 10.1088/1674-1137/42/6/064105 shu
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Received: 2017-11-10
Revised: 2018-04-02
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    This work is a part of the project INCT-FNA Proc. No. 464898/2014-5 and was partially supported by Conselho Nacional de Desenvolvimento Cientfico e Tecnolgico (CNPq), Brazil under grants 300602/2009-0 and 306786/2014-1. E. P. acknowledges support from the Israel Science Foundation. O. H. acknowledges the U.S. Department of Energy Office of Science, Office of Nuclear Physics program under award number DE-FG02-94ER40818

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The symmetry energy γ parameter of relativistic mean-field models

  • 1.  Departamento de Ciê
  • 2.  Universidade Federal do Rio de Janeiro, 27930-560, Macaé
  • 3.  Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
  • 4.  School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
  • 5.  Depto de Fí
  • Received Date: 2017-11-10
  • Accepted Date: 2018-04-02
  • Available Online: 2018-06-05
Fund Project:  This work is a part of the project INCT-FNA Proc. No. 464898/2014-5 and was partially supported by Conselho Nacional de Desenvolvimento Cientfico e Tecnolgico (CNPq), Brazil under grants 300602/2009-0 and 306786/2014-1. E. P. acknowledges support from the Israel Science Foundation. O. H. acknowledges the U.S. Department of Energy Office of Science, Office of Nuclear Physics program under award number DE-FG02-94ER40818

Abstract: The relativistic mean-field models tested in previous works against nuclear matter experimental values, critical parameters and macroscopic stellar properties are revisited and used in the evaluation of the symmetry energy γ parameter obtained in three different ways. We have checked that, independent of the choice made to calculate the γ values, a trend of linear correlation is observed between γ and the symmetry energy (S0) and a more clear linear relationship is established between γ and the slope of the symmetry energy (L0). These results directly contribute to the arising of other linear correlations between γ and the neutron star radii of R1.0 and R1.4, in agreement with recent findings. Finally, we have found that short-range correlations induce two specific parametrizations, namely, IU-FSU and DD-MEδ, simultaneously compatible with the neutron star mass constraint of 1.93≤Mmax/M⊙≤2.05 and with the overlap band for the L0×S0 region, to present γ in the range of γ=0.25±0.05.

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