Effects of the δ meson on the direct Urca processes in neutron stars

YU Zi; DING Wen-Bo

doi:10.1088/1674-1137/35/9/004

Chinese Physics C> 2011, Vol. 35> Issue(9) : 812-816 DOI: 10.1088/1674-1137/35/9/004

Effects of the δ meson on the direct Urca processes in neutron stars

YU Zi ^, ,
DING Wen-Bo

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In the framework of the relativistic mean field theory, the effects of the δ meson on the direct Urca (DURCA) processes are investigated. In a neutron star, the DURCA processes involving nucleons, Λ and Ξ^- can take place while the process involving the Ξ⁰ can not. With the inclusion of the δ meson, the threshold densities for the DURCA processes become lower. With the δ included, the threshold neutron star mass for the DURCA process among nucleons and electrons becomes smaller while the threshold masses for the processes involving hyperons become larger. When the δ meson is included, the total neutrino emissivity remarkably increases in the density range of 0.32--0.41 fm^-3. The total neutrino luminosity increases with the neutron star mass first and then decreases. The neutrino luminosity gets larger with the inclusion of the δ meson. The cooling of the EXO0748-676 is sensitive to the isovector scalar interaction.

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[1]

Page D, Lattimer J M, Prakash M et al. ApJS, 2004, 155: 6232 Heinke C O, Jonker P G, Wijnands R et al. ApJ, 2007, 660: 14243 Lattimer J M, Pethick C J, Prakash M et al. Phys. Rev. Lett., 1991, 66: 27014 Kubis S, Kutschera M. Nucl. Phys. A, 2003, 720:1895 Prakash M, Prakash M, Lattimer J M et al. ApJ, 1992, 390: L776 Kubis S. Phys. Rev. C, 2006, 73:0158057 DING W B, LIU G Z, ZHU M F et al. AA, 2009, 506: L13-L168 Yakovlev D G, Kaminker A D, Gnedin O Y et al. Phys. Rep., 2001, 354: 19 Leinson L B. Nucl. Phys. A, 2002, 707: 54310 LIU B, Greco V, Baran V et al. Phys. Rev. C, 2002, 65: 04520111 Kubis S, Kutschera M. Phys. Lett. B, 1997, 399: 19112 GUO H, CHEN Y J, LIU B et al. Phys. Rev. C, 2003, 68: 03580313 Menezes D P, Provid^encia C. Phys. Rev. C, 2004, 70: 05880114 WEI F X, MAO G J, KO C M et al. J. Phys. G, 2006, 32: 4715 LIU B, GUO H, Toro M D et al. Eur. Phys. J. A, 2005, 25: 29316 LIU B, Toro M D, Greco V et al. Phys. Rev. C, 2007, 75: 04880117 YU Z, LIU G Z, ZHU M F et al. Chin. Phys. Lett., 2009, 26: 02260118 Haensel P, Gnedie O Y. Astron. Astrophysics, 1994, 290: 458-46219 Batty C J, Friedman E, Gal A et al. Phys. Lett. B, 1994, 335: 27320 Balberg S, Gal A, Scha ner J. Prog. Theor. Phys. Suppl, 1994, 117: 32521 Stoks V G J, Lee T S H. Phys. Rev. C, 1999, 60: 02400622 Parmar A N, White N E, Giommi P et al. APJ, 1986, 308: 19923 Jansen F, Lumb D, Altieri B et al. Astr. Astrophys, 2001, 365: L1

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YU Zi and DING Wen-Bo. Effects of the δ meson on the direct Urca processes in neutron stars[J]. Chinese Physics C, 2011, 35(9): 812-816. doi: 10.1088/1674-1137/35/9/004

YU Zi and DING Wen-Bo. Effects of the δ meson on the direct Urca processes in neutron stars[J]. Chinese Physics C, 2011, 35(9): 812-816. doi: 10.1088/1674-1137/35/9/004 shu

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Received: 2010-11-08
Revised: 2010-12-30

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通讯作者: 陈斌, bchen63@163.com

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沈阳化工大学材料科学与工程学院沈阳 110142

Effects of the δ meson on the direct Urca processes in neutron stars

Corresponding author: YU Zi,

Received Date: 2010-11-08

Accepted Date: 2010-12-30

Available Online: 2011-09-05

Abstract: In the framework of the relativistic mean field theory, the effects of the δ meson on the direct Urca (DURCA) processes are investigated. In a neutron star, the DURCA processes involving nucleons, Λ and Ξ^- can take place while the process involving the Ξ⁰ can not. With the inclusion of the δ meson, the threshold densities for the DURCA processes become lower. With the δ included, the threshold neutron star mass for the DURCA process among nucleons and electrons becomes smaller while the threshold masses for the processes involving hyperons become larger. When the δ meson is included, the total neutrino emissivity remarkably increases in the density range of 0.32--0.41 fm^-3. The total neutrino luminosity increases with the neutron star mass first and then decreases. The neutrino luminosity gets larger with the inclusion of the δ meson. The cooling of the EXO0748-676 is sensitive to the isovector scalar interaction.

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