Effects of δ mesons on baryonic direct Urca processes inneutron star matter

  • This study investigates the relativistic neutrino emissivity of the nucleonic and hyperonic direct Urca processes in the degenerate baryon matter of neutron stars, within the framework of relativistic mean field theory. In particular, we study the influence of the isovector scalar interaction on the nucleonic and hyperonic direct Urca processes by exchanging δ mesons. The results indicate that δ mesons lead to obvious enhancement of the total neutrino emissivity, which must result in a more rapid cooling rate of neutron star matter.
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  • [1] Boguta J. Phys. Lett. B, 1981, 106: 255[2] Glendenning N K. Astrophys. J., 1985, 293: 470[3] Kaminker A D, Haensel P, Yakovlev D G. Astron. Astrophys. 2001, 373: L17[4] Leinson L B. Nucl. Phys. A, 2002, 707: 543[5] Yakovlev D G, Pethick C J. Ann. Rev. Astron. Astrophys., 2004, 42: 169[6] Prakash M, Prakash M, Lattimer J M, Pethick C J. Astrophys. J., 1992, 390: L77[7] Haensel P, Gnedin O Y. Astron. Astrophys., 1994, 290: 458[8] Yakovlev D G, Kaminker A D, Gnedin O Y, Haensel P. Phys. Rep., 2001, 354: 1[9] Schaffner J, Mishustin I N. Phys. Rev. C, 1996, 53: 1416[10] Bednarek I, Manka R. J. Phys. G: Nucl. Part. Phys., 2005, 31: 1009[11] MI A J, ZUO W, Burgio G et al. Chin. Phys. B, 2007, 16: 1934[12] DING W B, LIU G Z, ZHU M F et al. Chin. Phys. Lett., 2008, 25: 458[13] DING W B, LIU G Z, ZHU M F et al. Commun. Theor. Phys., 2010, 54: 500[14] XU Y, LIU G Z, WU Y R et al. Chin. Phys. Lett., 2011, 28: 079701[15] YU Z, DING W B. Commun. Theor. Phys., 2011, 55: 643[16] XU Y, LIU G Z, WANG H Y et al. Chin. Phys. Lett., 2012, 29[17] Kubis S, Kutschera M. Phys. Lett., B, 1997, 399: 191[18] Kubis S, Kutschera M, Stachniewicz S. Acta Phys. Pol. B, 1998, 29: 809[19] LIU B, Greco V, Baran V. Phys. Rev. C, 2002, 65: 045201[20] Menezes D P, Providência C. Phys. Rev. C, 2004, 70: 058801[21] LIU B, GUO H, di Toro M, Greco V. Eur. Phys. J. A, 2005, 25: 293[22] YU Z, LIU G Z, ZHU M F et al. Chin. Phys. Lett., 2009, 26: 022601[23] XU Y, LIU G Z, WU Y R et al. Plasma Sci. Technol., 2012, 14: 375[24] XU Y, LIU G Z, LIU C Z et al. Chin. Phys. Lett., 2013, 30: 062101[25] Leinson L B, Pérez A. Phys. Lett. B, 2001, 518: 15[26] Prakash M, Prakash M, Lattimer J M et al. The Astrophysical Journal, 1992, 390: L77[27] Schaab C, Balberg S, Schaffner-Bielich J. The Astrophysical Journal Letters, 1998, 504(2): L99[28] Tolman R C. Phys. Rev., 1939, 55: 364[29] Oppen- heimer J R. Volkoff G M. Phys. Rev., 1939, 55: 374
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HUANG Xiu-Lin, WANG Hai-Jun, LIU Guang-Zhou, LIU Cheng-Zhi and XU Yan. Effects of δ mesons on baryonic direct Urca processes inneutron star matter[J]. Chinese Physics C, 2015, 39(10): 105102. doi: 10.1088/1674-1137/39/10/105102
HUANG Xiu-Lin, WANG Hai-Jun, LIU Guang-Zhou, LIU Cheng-Zhi and XU Yan. Effects of δ mesons on baryonic direct Urca processes inneutron star matter[J]. Chinese Physics C, 2015, 39(10): 105102.  doi: 10.1088/1674-1137/39/10/105102 shu
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Received: 2015-10-21
Revised: 1900-01-01
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Effects of δ mesons on baryonic direct Urca processes inneutron star matter

    Corresponding author: XU Yan,

Abstract: This study investigates the relativistic neutrino emissivity of the nucleonic and hyperonic direct Urca processes in the degenerate baryon matter of neutron stars, within the framework of relativistic mean field theory. In particular, we study the influence of the isovector scalar interaction on the nucleonic and hyperonic direct Urca processes by exchanging δ mesons. The results indicate that δ mesons lead to obvious enhancement of the total neutrino emissivity, which must result in a more rapid cooling rate of neutron star matter.

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