Chinese Physics C > 2004, Vol. 28 > Issue(S1): 99-101

Direct URCA Process in Neutron Stars

School of Physics, Peking University, Beijing 100871, China2 Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100871, China3 Center of Theoretical Nuclear Physics, National Laboratory of Heavey Ion Accelerator, Lanzhou 730000, China4 Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

Abstract
HTML
Reference
Related

PDF

Abstract：
The onset of the most powerful neutrino emission candidate in the cooling of neutron stars, direct URCA process, requires a high threshold proton fraction. The proton fraction in neutron stars relies on the isospin dependent part of nuclear force, which can be constrained by the measurement of the neutron skin thickness in heavy nuclei such as ²⁰⁸Pb. Adding new isospin dependent correction terms to the effective interactions PK1, NL3, S271 and Z271, the correlation between the proton fraction and neutron skin thickness in ²⁰⁸Pb is studied. For a neutron star with fixed mass, the central proton fraction increases with increasing predicted values of neutron skin thickness in ²⁰⁸Pb.

References

[1]

. Lattimer J M, Pethick C J, Prakash M et al. Phys. Rev. Lett., 1991, 66: 27012.Pavlov G G, Kargaltsev O Y, Sanwal D et al. Astrophys. J. Lett., 2001, 554: L1893.Typel S, Brown B A. Phys. Rev., 2001, C64: 0273024.Jerson Laboratory Experiment E-00-003, Spokespersons Michaels R, P. Souder A., Urciuoli G. M.5.SHEN G, LI J, Hillhouse G C et al. accepted by Phys.Rev. C6.MENG J, RING P. Phys. Rev. Lett., 1996, 77: 39637.MENG J. Nucl. Phys., 1998, A635: 38.MENG J, RING P. Phys. Rev. Lett., 1998, 80: 4609.Horowitz C J, Piekarewicz J. Phys. Rev., 2002, C66:05580310.LONG W H, MENG J, Giai N V et al. Phys. Rev., 2004,C69: 03431911.Lalazissis G A, Knig J, RING P. Phys. Rev., 1997, C55:54012.Oppenheimer J R, Volkoff G M. Phys. Rev., 1939, 55: 374

[1]	YU Zi,DING Wen-Bo. Effects of the δ meson on the direct Urca processes in neutron stars. Chinese Physics C, 2011, 35(9): 812-816.doi:10.1088/1674-1137/35/9/004
[2]	ZHAO Xian-Feng,WANG Shun-Jin,ZHANG Hua,JIA Huan-Yu. Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature. Chinese Physics C, 2007, 31(6): 532-537.
[3]	ZHAO Xian-Feng,WANG Shun-Jin,ZHANG Hua,JIA Huan-Yu. Effect of f₀(975) and φ(1020) Mesons on Neutron Star Mater. Chinese Physics C, 2007, 31(4): 345-349.
[4]	CHEN Wei. Thermal Property of Protoneutron Star Matter. Chinese Physics C, 2006, 30(2): 118-122.
[5]	ZUO Wei,LI Ang,LUO Pei-Yan,YONG Gao-Chan. Properties of Proto-Neutron Star and Effect of Three-Body Forces. Chinese Physics C, 2006, 30(10): 956-960.
[6]	DING Wen-Bo,LIU Guang-Zhou. Condensations of K^－and K⁰in Neutron Star Matter. Chinese Physics C, 2006, 30(S2): 249-251.
[7]	WEN Hai-Bao. Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars. Chinese Physics C, 2005, 29(7): 657-663.
[8]	CHEN Wei,LIU Liang-Gang. The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields. Chinese Physics C, 2005, 29(2): 119-123.
[9]	ZUO Wei,LI Ang,CHEN Ji-Yan,LI Zeng-Hua. Kaon Condensation in Neutron Star Matter and Nuclear Three-Body Force Effect. Chinese Physics C, 2005, 29(7): 632-638.
[10]	ZHU Zhao-Huan,BAN Shu-Fang,LI Jun,MENG Jie. Pesponse of the Neutron Star Properties to the Equation of State at Low Density. Chinese Physics C, 2005, 29(6): 565-569.
[11]	LI Jun,BAN Shu-Fang,JIA Huan-Yu,SANG Jian-Ping,MENG Jie. Description of the Nuclear Matter and Neutron Star in Relativistic Mean Field Theory with Density-Dependent Interactions. Chinese Physics C, 2004, 28(2): 140-147.
[12]	ZHANG Miao-Jing,ZHANG Bo,LIU Ji-Hong,LI Guang-Lie. Abundances of Metal-Poor Stars and Slow Neutron-Capture Progress. Chinese Physics C, 2003, 27(4): 304-308.
[13]	JIA Huan-Yu,MENG Jie,ZHAO En-Guang,LI Jun,SANG Jian-Ping. Effect of Temperature on Hyperon Neutron Star. Chinese Physics C, 2003, 27(3): 200-205.
[14]	LIU Bo,GUO Hua. In-Medium Effects on Neutron Stars. Chinese Physics C, 2003, 27(8): 683-687.
[15]	GUO Hua,LIU Bo,LI Xi-Guo,CHEN Yan-Jun. Kaon Condensation in Neutron Star Matter. Chinese Physics C, 2003, 27(2): 113-117.
[16]	JIA Huan-Yu,LV Hong-Feng,MENG Jie. Hyperon rms Radii of_Λ²⁰⁸Pb and Neutron Star Structure. Chinese Physics C, 2002, 26(10): 1050-1055.
[17]	LI Wen-Fei,ZHANG Feng-Shou,CHEN Lie-Wen. Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter. Chinese Physics C, 2001, 25(9): 877-883.
[18]	LI Wen-Fei,ZHANG Feng-Shou,CHEN Lie-Wen. On the Moment of Inertia and Surface Redshift of Neutron Star. Chinese Physics C, 2001, 25(10): 1006-1011.
[19]	LI Wen-Fei , 2< sup>,ZHANG Feng-Shou , CHEN Lie-Wen . Density Dependence of Proton Fraction in Neutron Stars. Chinese Physics C, 2001, 25(8): 759-764.
[20]	SUN Bao-Xi,JIA Huan-Yu,MENG Jie,ZHAO En-Guang. Neutron Star in Relativistic Mean-field Approximation. Chinese Physics C, 2000, 24(S1): 69-72.

Access

Get Citation

SHEN Gang, MENG Jie and Hillhouse G. Direct URCA Process in Neutron Stars[J]. Chinese Physics C, 2004, 28(S1): 99-101.

SHEN Gang, MENG Jie and Hillhouse G. Direct URCA Process in Neutron Stars[J]. Chinese Physics C, 2004, 28(S1): 99-101. shu

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2004-12-30
Revised: 1900-01-01

Article Metric

Article Views(4259)
PDF Downloads(605)
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

Direct URCA Process in Neutron Stars

Corresponding author:MENG Jie,

School of Physics, Peking University, Beijing 100871, China2 Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100871, China3 Center of Theoretical Nuclear Physics, National Laboratory of Heavey Ion Accelerator, Lanzhou 730000, China4 Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

Received Date:2004-12-30
Accepted Date:1900-01-01
Available Online:2004-04-02

Abstract:The onset of the most powerful neutrino emission candidate in the cooling of neutron stars, direct URCA process, requires a high threshold proton fraction. The proton fraction in neutron stars relies on the isospin dependent part of nuclear force, which can be constrained by the measurement of the neutron skin thickness in heavy nuclei such as²⁰⁸Pb. Adding new isospin dependent correction terms to the effective interactions PK1, NL3, S271 and Z271, the correlation between the proton fraction and neutron skin thickness in²⁰⁸Pb is studied. For a neutron star with fixed mass, the central proton fraction increases with increasing predicted values of neutron skin thickness in²⁰⁸Pb.