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

Abstract
HTML
Reference
Related

PDF

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.

References

[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

[1]	Ting-Ting Sun , Cheng-Jun Xia , Shi-Sheng Zhang , M. S. Smith . Massive neutron stars and Λ-hypernuclei in relativistic mean field models. Chinese Physics C, 2018, 42(2): 025101. doi: 10.1088/1674-1137/42/2/025101
[2]	A. H. Farajian , M. Bigdeli , S. Belbasi . LOCV calculation of the equations of state and properties of rapidly rotating neutron stars. Chinese Physics C, 2018, 42(6): 065102. doi: 10.1088/1674-1137/42/6/065102
[3]	Liuyuan Shen , Yicen Mou , Yunlong Zheng , Mingzhe Li . Direct couplings of mimetic dark matter and their cosmological effects. Chinese Physics C, 2018, 42(1): 015101. doi: 10.1088/1674-1137/42/1/015101
[4]	Cui Zhu , Xia Zhou , Na Wang . Rotational energy conversion and thermal evolution of neutron stars. Chinese Physics C, 2017, 41(12): 125104. doi: 10.1088/1674-1137/41/12/125104
[5]	Fei Wu , Chen Wu , Zhong-Zhou Ren . Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments. Chinese Physics C, 2017, 41(4): 045102. doi: 10.1088/1674-1137/41/4/045102
[6]	Nai-Bo Zhang , Shou-Yu Wang , Bin Qi , Jian-Hua Gao , Bao-Yuan Sun . Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars. Chinese Physics C, 2017, 41(7): 075101. doi: 10.1088/1674-1137/41/7/075101
[7]	HUANG Xiu-Lin , WANG Hai-Jun , LIU Guang-Zhou , LIU Cheng-Zhi , XU Yan . Effects of δ mesons on baryonic direct Urca processes inneutron star matter. Chinese Physics C, 2015, 39(10): 105102. doi: 10.1088/1674-1137/39/10/105102
[8]	ZHOU Xia , KANG Miao , WANG Na . Effect of magnetic field decay on the chemical heating of cooling neutron stars. Chinese Physics C, 2013, 37(8): 085102. doi: 10.1088/1674-1137/37/8/085102
[9]	CHEN Ya-Zheng , CHEN Jun-Mou , LUO Yan-An , SHEN Hong , LI Xue-Qian . Effects of nuclear deformation on the form factorfor direct dark matter detection. Chinese Physics C, 2012, 36(6): 505-512 . doi: 10.1088/1674-1137/36/6/005
[10]	WEI Wei , CHEN Lei-Lei . Rotochemical heating in hybrid stars withmodified Urca reactions in operation. Chinese Physics C, 2012, 36(7): 601-604. doi: 10.1088/1674-1137/36/7/006
[11]	PI Chun-Mei , YANG Shu-Hua , ZHOU Xia , ZHOU Ai-Zhi . Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source. Chinese Physics C, 2010, 34(12): 1818-1822. doi: 10.1088/1674-1137/34/12/006
[12]	KANG Miao , ZHOU Xia , WANG Xiao-Dong , HENG Yao-Fu . Influence of medium effects on the rotating hybrid stars. Chinese Physics C, 2010, 34(11): 1696-1699. doi: 10.1088/1674-1137/34/11/005
[13]	ZHANG Yuan-Jiang , LI Gang , ZHAO Qiang . Manifestation of intermediate meson loop effects in charmonium decays. Chinese Physics C, 2010, 34(9): 1181-1184. doi: 10.1088/1674-1137/34/9/006
[14]	LIU Xiao-Jin , WU Chen , REN Zhong-Zhou . Effects of the density dependence of the symmetry energy on neutron stars. Chinese Physics C, 2010, 34(11): 1709-1713. doi: 10.1088/1674-1137/34/11/008
[15]	HUANG Fei . Hadro- and photo-production of η' in quasi-free proton and neutron processes. Chinese Physics C, 2009, 33(12): 1291-1295. doi: 10.1088/1674-1137/33/12/040
[16]	LIU Jun , JIA Wen-Zhi , WANG Shun-Jin . Microscopic calculation of the magnetic field of neutron stars. Chinese Physics C, 2009, 33(9): 737-742. doi: 10.1088/1674-1137/33/9/005
[17]	LIU Jing-Jing , LUO Zhi-Quan . Neutrino energy loss by electron capture in magnetic field at the crusts of neutron stars. Chinese Physics C, 2008, 32(2): 108-111. doi: 10.1088/1674-1137/32/2/007
[18]	YANG Fang , SHEN Hong . Hadron-quark phase transition in neutron stars. Chinese Physics C, 2008, 32(S2): 77-80.
[19]	SHEN Gang , MENG Jie , Hillhouse G . Direct URCA Process in Neutron Stars. Chinese Physics C, 2004, 28(S1): 99-101.
[20]	Yu Hong , Shen Qixing , Zhang Lin . Angular Distribution of Processes e⁺e^-→τ⁺τ^-,τ^-→a₁^-υ_τ,a₁^-→ρπ and Characteristics of a₁ Meson. Chinese Physics C, 1994, 18(S2): 141-150.

Access

Get Citation

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

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

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

Article Metric

Article Views(2434)
PDF Downloads(446)
Cited by(0)

Policy on re-use

To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.

通讯作者: 陈斌, bchen63@163.com

1.
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.

HTML

Reference (1)

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

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article