Chinese Physics C > 2017, Vol. 41 > Issue(12): 125104 DOI: 10.1088/1674-1137/41/12/125104

Rotational energy conversion and thermal evolution of neutron stars

Cui Zhu^1,2,3,
Xia Zhou^1,2,,,
Na Wang^1,2

1.
Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China
2.
Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, China
3.
University of Chinese Academy of Sciences, 19 A Yuquan Road, Beijing 100049, China

Abstract
HTML
Reference
Related

PDF

Abstract：
Pulsars are rapidly spinning, strongly magnetized neutron stars. Their electromagnetic dipole radiation is usually assumed to be at the expense of the rotational energy. In this work, we consider a new channel through which rotational energy could be radiated away directly via neutrinos. With this new energy conversion channel, we can improve the chemical heating mechanism that originates in the deviation from β equilibrium due to spin-down compression. The improved chemical and thermal evolution equations with different magnetic field strengths are solved numerically. The results show that the new energy conversion channel could raise the surface temperature of neutron stars, especially for weak field stars at later stages of their evolution. Moreover, our results indicate that the new energy conversion channel induced by the non-equilibrium reaction processes should be taken into account in the study of thermal evolution.
- neutron star,
- rotation,
- thermal evolution,
- energy conversion

References

[1]	W. Becker, Neutron Stars and Pulsars, Astrophys. Space Sci. Library, Vol 357 (New-York:Springer, 2008)
[2]	N. K. Glendenning, Compact Stars:Nuclear Physics, Particle Physics, and General Relativity (New-York:Springer, 2000)
[3]	X. P. Zheng, X. Zhou, Mon. Not. R. Astron. Soc., 371, 1659 (2006)
[4]	R. Negreiros, S. Schramm, and F. Weber, Phys. Lett. B, 718:1176 (2013)
[5]	A. Reisenegger, Astrophys. J, 442:749 (1995)
[6]	K. S. Cheng and Z. G. Dai, Astrophys. J, 468:819 (1996)
[7]	R. Fernndez and A. Reisenegger, Astrophys. J, 625:291 (2005)
[8]	K. Iida, K. Sato, Astrophys. J, 477, 294 (1997)
[9]	K. S. Cheng, W. Y. Chau, J. L. Zhang, and H. F. Chau, Astrophys. J, 396:135 (1992)
[10]	Y. W. Yu and X. P. Zheng, Astron. Astrophys., 450:1071 (2006)
[11]	X. P. Zheng and Y. W. Yu, Astron. Astrophys., 445:627 (2006)
[12]	X. Zhou, L. Z. Wang, and A. Z. Zhou, Pub. Astron. Soc. Pac., 119:1367 (2007)
[13]	X. P. Zheng, X. Zhou, and S. H. Yang, Physics Letters B, 729:79 (2014)
[14]	B. A. Sa'd and J. Schaffner-Bielich, arXiv:0908.4190
[15]	S. H. Yang, X. P. Zheng, and C. M. Pi, Phys. Lett. B, 683:255 (2009)
[16]	S. H. Yang, X. P. Zheng, C. M. Pi, and Y. W. Yu, Mon. Not. R. Astron. Soc., 403:2007 (2010)
[17]	C. M. Pi, S. H. Yang, and X. P. Zheng, Chinese Physics Letters, 28(10):109701 (2011)
[18]	P. Jaikumar and S. Sandalski, Phys. Rev. D, 82:103013 (2010)
[19]	A. Finzi and R. A. Wolf, Astrophys. J, 153:835 (1968)
[20]	P. Haensel, Astron. Astrophys., 262, 131 (1992)
[21]	E. Gourgoulhon and P. Haensel, Astron. Astrophys., 271:187 (1993)
[22]	P. Jofr, A. Reisenegger, and R. Fernndez, Phys. Rev. Lett., 97:131102 (2006)
[23]	D. G. Yakovlev, A. D. Kaminker, O. Y. Gnedin, and P. Haensel, Phys. Rep., 354:1 (2001)
[24]	C. Petrovichand and A. Reisenegger, Astron. Astrophys., 521:A77 (2009)
[25]	N. Gonzalez-Jimenez, C. Petrovich, and A. Reisenegger, Mon. Not. R. Astron. Soc., 447:2073 (2015)
[26]	M. Prakash, T. Ainsworth, and J. M. Lattimer, Phys. Rev. Lett., 61:2518 (1988)
[27]	E. H. Gudmundsson, C. J. Pethick, and R. I. Epstein, ApJ, 272:286 (1983)
[28]	A. Y. Potekhin, D. G. Yakovlev, and P. Prakash. A A, 374:213 (2001)
[29]	P. Haensel, Astron. Astrophys., 262:131 (1992)
[30]	S. Mahmoodifar and T. Strohmayer, Astrophys. J., 840:94 (2017)
[31]	K. Schwenzer, T. Boztepe, T. Gver, and E. Vurgun, Mon. Not. R. Astron. Soc., 466:2560 (2017)
[32]	B. Rangelov et al, Astrophys. J., 835:264 (2017)

[1]	Sunil Kumar,Vikesh Kumar,Pankaj Kumar,Raj Kumar,Shashi K Dhiman. Nuclear matter and neutron star properties constrained by CREX results and astrophysical constraints: A covariance study. Chinese Physics C, 2025, 49(7): 074109.doi:10.1088/1674-1137/adc65b
[2]	Fei Sun,Shuang Li,Rui Wen,Anping Huang,Wei Xie. Rotation effect on the thermodynamics of QCD matter. Chinese Physics C, 2025, 49(9): 093105.doi:10.1088/1674-1137/add25e
[3]	Minghua Wei,Yin Jiang,Mei Huang. Mass splitting of vector mesons and spontaneous spin polarization under rotation. Chinese Physics C, 2022, 46(2): 024102.doi:10.1088/1674-1137/ac338e
[4]	Houyuan Chen,Dehua Wen,Na Zhang. Suitable resolution of EOS tables for neutron star investigations. Chinese Physics C, 2019, 43(5): 054108.doi:10.1088/1674-1137/43/5/054108
[5]	Zhao-Ming Zeng,Hui Gong,Jian-Min Li,Qian Yue,Zhi Zeng,Jian-Ping Cheng. Design of the thermal neutron detection system for CJPL-II. Chinese Physics C, 2017, 41(5): 056002.doi:10.1088/1674-1137/41/5/056002
[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]	Ke Li,Jian-Rong Zhou,Xiao-Dong Wang,Tao Xiong,Ying Zhang,Yu-Guang Xie,Liang Zhou,Hong Xu,Gui-An Yang,Yan-Feng Wang,Yan Wang,Jin-Jie Wu,Zhi-Jia Sun,Bi-Tao Hu. Study of a nTHGEM-based thermal neutron detector. Chinese Physics C, 2016, 40(7): 076002.doi:10.1088/1674-1137/40/7/076002
[8]	YANG Lei,ZHOU Jian-Rong,SUN Zhi-Jia,ZHANG Ying,HUANG Chao-Qiang,SUN Guang-Ai,WANG Yan-Feng,YANG Gui-An,XU Hong,XIE Yu-Guang,CHEN Yuan-Bo. Experimental research on a THGEM-based thermal neutron detector. Chinese Physics C, 2015, 39(5): 056002.doi:10.1088/1674-1137/39/5/056002
[9]	BAI Zhi-Jun,FU Xi-Ming,JIAO Chang-Feng,XU Fu-Rong. Shape coexistence and evolution in neutron-deficient krypton isotopes. Chinese Physics C, 2015, 39(9): 094101.doi:10.1088/1674-1137/39/9/094101
[10]	DING Wen-Bo,YU Zi,MI Geng,WANG Chun-Yan. Neutron star cooling in various sets of nucleon coupling constants. Chinese Physics C, 2013, 37(5): 055101.doi:10.1088/1674-1137/37/5/055101
[11]	LIU Ye,MA Xin-Hua,ZHAO Jing. Thermal neutron flux produced by EAS at various altitudes. Chinese Physics C, 2013, 37(1): 015001.doi:10.1088/1674-1137/37/1/015001
[12]	WENG Ming-Hua,GUO Xin-Heng,LIU Bo. Vacuum fluctuation effects on hyperonic neutron star matter. Chinese Physics C, 2013, 37(12): 125101.doi:10.1088/1674-1137/37/12/125101
[13]	TIAN Yang,YANG Yi-Gang,LI Yu-Lan,LI Yuan-Jing. A numerical model of a coated capillary-plate thermal neutron collimator. Chinese Physics C, 2012, 36(5): 438-442.doi:10.1088/1674-1137/36/5/010
[14]	ZHAO Xian-Feng,ZHANG Hua,JIA Huan-Yu. On the moment of inertia of a proto neutron star. Chinese Physics C, 2010, 34(10): 1587-1592.doi:10.1088/1674-1137/34/10/007
[15]	QIAN Sen,WANG Yi-Fang,ZHANG Jia-Wen,LI Jin,CHEN Yuan-Bo,CHEN Jin,WANG Zhi-Gang,MA Lie-Hua. Study of the RPC-Gd as thermal neutron detector. Chinese Physics C, 2009, 33(9): 769-773.doi:10.1088/1674-1137/33/9/011
[16]	LI Ang,PENG Guang-Xiong,Lombardo U. Deconfinement phase transition in neutron star matter. Chinese Physics C, 2009, 33(S1): 61-63.doi:10.1088/1674-1137/33/S1/020
[17]	ZHOU Li-Juan,ZHANG Ben-Wei,ZHANG Han-Zhong,WANG En-Ke. Jet-photon conversion with energy loss in heavy ion collisions. Chinese Physics C, 2009, 33(3): 201-204.doi:10.1088/1674-1137/33/3/008
[18]	CHEN Yong-Shou,GAO Zao-Chun. Triaxial rotation in atomic nuclei. Chinese Physics C, 2009, 33(S1): 1-4.doi:10.1088/1674-1137/33/S1/001
[19]	YUE Peng,SHEN Hong. Antikaon condensation in neutron star matter with strong magnetic fields. Chinese Physics C, 2008, 32(S2): 85-88.
[20]	HE Chuang-Ye,ZHU Li-Hua,WU Xiao-Guang,WEN Shu-Xian,LI Guang-Sheng,LIU Ying,WANG Zhi-Min,LI Xue-Qin,CUI Xing-Zhu,SUN Hui-Bin,MA Rui-Guang,YANG Chun-Xiang. Magnetic rotation in¹⁰⁶Ag. Chinese Physics C, 2008, 32(S2): 120-123.

Access

Get Citation

Cui Zhu, Xia Zhou and Na Wang. Rotational energy conversion and thermal evolution of neutron stars[J]. Chinese Physics C, 2017, 41(12): 125104. doi: 10.1088/1674-1137/41/12/125104

Cui Zhu, Xia Zhou and Na Wang. Rotational energy conversion and thermal evolution of neutron stars[J]. Chinese Physics C, 2017, 41(12): 125104. doi:10.1088/1674-1137/41/12/125104 shu

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2017-04-07
Revised: 2017-09-11

Fund

Supported by National Natural Science Foundation of China (11373006) and the West Light Foundation of Chinese Academy of Sciences (ZD201302)

Article Metric

Article Views(3694)
PDF Downloads(37)
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

Rotational energy conversion and thermal evolution of neutron stars

Corresponding author:Xia Zhou,

1. Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China

2. Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, China

3. University of Chinese Academy of Sciences, 19 A Yuquan Road, Beijing 100049, China

Received Date:2017-04-07

Accepted Date:2017-09-11

Available Online:2017-12-05

Fund Project:Supported by National Natural Science Foundation of China (11373006) and the West Light Foundation of Chinese Academy of Sciences (ZD201302)

Abstract:Pulsars are rapidly spinning, strongly magnetized neutron stars. Their electromagnetic dipole radiation is usually assumed to be at the expense of the rotational energy. In this work, we consider a new channel through which rotational energy could be radiated away directly via neutrinos. With this new energy conversion channel, we can improve the chemical heating mechanism that originates in the deviation from β equilibrium due to spin-down compression. The improved chemical and thermal evolution equations with different magnetic field strengths are solved numerically. The results show that the new energy conversion channel could raise the surface temperature of neutron stars, especially for weak field stars at later stages of their evolution. Moreover, our results indicate that the new energy conversion channel induced by the non-equilibrium reaction processes should be taken into account in the study of thermal evolution.

HTML

Reference (32)

Rotational energy conversion and thermal evolution of neutron stars

Abstract：

References

Access

Article Metrics

Metrics

通讯作者:陈斌, bchen63@163.com

Email This Article