Effects of strong magnetic field on moment of inertia and surface gravitational redshift in neutron star

Zhao Shi-Yi; Liu Cheng-Zhi; Huang Xiu-Lin; Wang Yi-Bo; Xu Yan

doi:10.7498/aps.70.20211051

Abstract

Research on the properties of neutron stars with strong magnetic fields is of great significance in constraining the equation of state and revealing the real distribution of magnetic fields in neutron stars. The main macroscopic properties of the traditional neutron star matter under β equilibrium condition are studied within the relativistic mean field theory through using the GL91 parameter set by considering the strong magnetic field. It is found that the onset of the strong magnetic field leads to the stiffened equation of state of the traditional neutron star matter. The maximum mass of the traditional neutron star grows from 2.111 M_⊙ to 3.081 M_⊙, the radius of the fixed mass traditional neutron star grows larger with the increase of internal magnetic field, which makes traditional neutron star become less dense. The strong magnetic field can also reduce the surface gravitational redshift and strengthen the moment of inertia of the traditional neutron star matter. In addition, the theoretical ranges of the surface gravitational redshift and the moment of inertia for the four massive PSRs J1614-2230, J0348+0432, J0740+6620 and J2215-5135, and the 2.50 M_⊙ − 2.67 M_⊙ compact object in the binary merger event GW190814 are also given. The results show that the ranges of the surface redshift become narrower, while the scopes of the moment of inertia widen as the magnetizing field increases in the five stars.

Keywords:

Authors and contacts

1.
Changchun Observatory, National Astronomical Observatories, Chinese Academy of Sciences, Changchun 130117, China
2.
School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing 100049, China

Corresponding author: Liu Cheng-Zhi, lcz@cho.ac.cn ; Wang Yi-Bo, wangyb@cho.ac.cn ; Xu Yan, xuy@cho.ac.cn

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 11805022, 11803057).

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References

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Cited By

图 1 不同磁场强度下(α = 0, 20, 40, 60)中子星物质的(a)压强-核子密度、(b)质量-半径关系. 本文中, 黑红绿蓝四条线表示α = 0, 20, 40, 60四种情况; 不同颜色条纹区域分别表示PSRs J1614-2230, J0348+0432, J0740+6620, J2215-5135以及GW190814中致密星的质量测量值范围; 橙色误差棒表示NICER公布的PSR J0030+0415的质量-半径测量值对中子星质量-半径关系的约束. 各曲线上黑色圆点表示中子星最大质量所处位置, 三角形点表示最大半径所处位置

Figure 1. Relationship of (a) the pressure - density and (b) the mass - radius in neutron star (NS) matter. In the paper the black, red, green, and blue lines represent the four cases of α = 0, 20, 40 and 60, respectively. The different colored areas stand for the recent constraints inferred from PSRs J1614-2230, J0348+0432, J0740+6620, J2215-5135 and GW190814 respectively. The orange error bar represents the constraints on the mass-radius limits of PSR J0030+0451 obtained from NICER observations. The dots and the triangle points show the maximum masses and radii of NSs for the four cases, respectively.

DownLoad: Full-Size Img PowerPoint

图 2 不同磁场强度下(α = 0, 20, 40, 60), 中子星内声速-核子密度关系

Figure 2. Relationships of the speed of sound and the nucleon density with α = 0, 20, 40, 60 in NS matter.

DownLoad: Full-Size Img PowerPoint

图 3 不同磁场强度下(α = 0, 20, 40, 60), 中子星转动惯量-质量关系

Figure 3. Relationships of the moment of inertia and the mass with α = 0, 20, 40, 60 in NS matter.

DownLoad: Full-Size Img PowerPoint

图 4 不同磁场强度下(α = 0, 20, 40, 60), 中子星表面引力红移-质量的关系

Figure 4. Relationships of the gravitational redshift and mass with α = 0, 20, 40, 60 in NS matter.

DownLoad: Full-Size Img PowerPoint

表 1 不同磁场强度下(α = 0, 20, 40, 60), 中子星最大质量及其对应半径和中心密度, 最大半径及其对应质量和中心密度

Table 1. Table 1. Values of the maximum NS masses M_max and the corresponding radii R as well as the center densities ρ_c/ρ₀, values of the maximum NS radii R_max and the corresponding masses M as well as the center densities ρ_c/ρ₀ with α = 0, 20, 40, 60 in npeμ matter.

α	中子星最大质量处			中子星最大半径处
α	M /M_⊙	R /km	ρ_c/ρ₀	M /M_⊙	R/km	ρ_c/ρ₀
0	2.111	11.648	7.013	0.971	14.014	2.102
20	2.574	12.496	3.977	1.520	14.306	2.227
40	2.877	13.601	2.960	2.066	15.060	2.031
60	3.081	14.375	2.478	2.415	15.765	1.734

DownLoad: CSV

表 2 不同磁场强度下(α = 0, 20, 40, 60), PSRs J1614-2230, J0348+0432, J0740+6620, J2215-5135以及GW190814中致密星的半径、转动惯量、引力红移理论值范围

Table 2. Ranges of the theoretical values for the radius, the moment of inertia and the gravitational redshift corresponding to PSRS J1614-2230, J0348+0432, J0740+6620, J2215-5135 and the compact star in GW190814 with α = 0, 20, 40, 60.

Source	α	R/km	I/M_⊙·km²	Z
PSR J1614-2230	0	[13.067, 13.158]	[131.615, 133.926]	[0.317, 0.329]
	20	[14.179, 14.220]	[148.276, 152.485]	[0.283, 0.291]
	40	[15.037, 15.048]	[161.795, 166.371]	[0.261, 0.269]
	60	[15.450, 15.670]	[172.197, 175.693]	[0.244, 0.253]
PSR J0348-0432	0	[12.548, 12.954]	[135.781, 138.653]	[0.348, 0.388]
	20	[14.108, 14.179]	[155.490, 164.997]	[0.305, 0.323]
	40	[15.048, 15.068]	[171.237, 182.428]	[0.277, 0.291]
	60	[15.690, 15.722]	[182.428, 195.897]	[0.260, 0.276]
PSR J0740+6620	0	[11.648, 12.965]	[119.641, 138.653]	[0.344, 0.462]
	20	[13.782, 14.170]	[155.490, 194.213]	[0.300, 0.416]
	40	[14.976, 15.060]	[171.237, 220.062]	[0.273, 0.361]
	60	[15.670, 15.783]	[182.428, 238.087]	[0.259, 0.334]
PSR J2215-5135	0	—	—	—
	20	[13.679, 13.986]	[180.150, 198.670]	[0.362, 0.429]
	40	[14.987, 15.037]	[199.859, 226.797]	[0.325, 0.371]
	60	[15.742, 15.783]	[215.606, 244.822]	[0.300, 0.343]
GW190814	0	—	—	—
	20	[12.496, 13.291]	[203.820, 206.593]	[0.496, 0.591]
	40	[14.670, 14.905]	[242.544, 264.431]	[0.407, 0.470]
	60	[15.670, 15.752]	[262.153, 288.002]	[0.370, 0.418]

DownLoad: CSV

[1]	Riley T E, Watts A L, Bogdanov S, et al. 2019 Astrophys. J. Lett. 887 21 Google Scholar
[2]	Shao D H, Tang S P, Jiang J L, et al. 2020 Phys. Rev. D 102 063006 Google Scholar
[3]	Zhao X F 2020 Chin. J. Phys. 63 240 Google Scholar
[4]	喻传赞 1980 科学通报 16 50 Google Scholar Yu C Z 1980 Chin. Sci. Bull. 16 50 Google Scholar
[5]	陈家麟, 季沛勇 2013 上海大学学报(自然科学版) 19 176 Google Scholar Chen J L, Ji P Y 2013 Journal of Shanghai University (Natural science Edition) 19 176 Google Scholar
[6]	彭芳, 彭秋和, 张丰收 2001 天文学报 42 1 Google Scholar Peng F, Peng Q H, Zhang F S 2001 Acta Astronomica Sinica 42 1 Google Scholar
[7]	赵先锋, 张华 2010 四川大学学报(自然科学版) 4 28 Google Scholar Zhao X F, Zhang H 2010 Journal of Sichuan University (Natural Science Edition) 4 28 Google Scholar
[8]	Zhao X F 2020 Chin. J. Physics 63 240
[9]	Lim Y, Holt J W, Stahulak R J 2019 Phys. Rev. C 3 035802 Google Scholar
[10]	Sen D 2021 J. Phys. G 48 025201 Google Scholar
[11]	Wang W, Tang Y M, Tuo Y L 2021 J. High. Energy Astrophys. 30 1 Google Scholar
[12]	Kouvelioton C 1998 Nature 393 253 Google Scholar
[13]	Kaspi V M 2003 Astrophys. J. 588 93 Google Scholar
[14]	Shapiro S L 1983 Black Holes, White Dwarfs and neutron Stars (New York: Wiley - Insterscience) pp277−282
[15]	Lai D, Shapiro S L 1991 Astrophys. J. 383 745 Google Scholar
[16]	孙晓辉, 韩金林 2002 天文学进展 20 130 Google Scholar Sun X H, Han J L 2002 Prog. Astron. 20 130 Google Scholar
[17]	Chakrabarty S, Debades B, Subrata P 1997 Phys. Rev. Lett. 78 2898 Google Scholar
[18]	Broderick A, Prakash M, Lattimer J M 2000 Astrophys. J. 537 351 Google Scholar
[19]	Broderick A E, Prakash M, Lattimer J M 2002 Phys. Lett. B 531 167 Google Scholar
[20]	Bednarek I, Brzezina A, Manka R 2003 Nucl. Phys. A 24 245 Google Scholar
[21]	Mao G J, Akira 2003 Chin. J. Astron. Astrophys. 3 359 Google Scholar
[22]	张洁, 刘门全, 魏丙涛, 罗志全 2008 物理学报 57 5448 Google Scholar Zhang J, Liu M Q, Wei B T, Luo Z Q 2008 Acta Phys. Sin. 57 5448 Google Scholar
[23]	Dong J M, Lombardo U, Zuo W 2013 Nucl. Phys. A 898 32 Google Scholar
[24]	Dong J M, Zuo W, Gu J Z 2016 Sci. China Phys. Mech. 59 642003 Google Scholar
[25]	鲍世绍, 胡金牛, 申虹 2018 科学通报 63 828 Google Scholar Bao S S, Hu J N, Shen H 2018 Chin. Sci. Bull. 63 828 Google Scholar
[26]	Boguta J, Bodmer A R 1977 Nucl. Phys. 292 413 Google Scholar
[27]	Glendenning N K, Moszkowski S A 1991 Phys. Rev. Lett. 67 2414 Google Scholar
[28]	Glendenning N K 1992 Phys. Rev. D 46 1274 Google Scholar
[29]	朗道著 (周奇译)1 963 连续媒介电动力学 (北京: 人民教育出版社) 第179—182页 Landau L D, Lifshitz E M, Pitaevskii L P (translated by Zhou Q) 1963 Electrodynamics of Continuous Media (Beijing: People’s Education Press) pp179−182 (in Chinese)
[30]	Oppenheimer J R, Volkoff G M 1939 Phys. Rev. 55 374 Google Scholar
[31]	Tolman R C 1939 Phys. Rev. 55 364 Google Scholar
[32]	Worley A, Krastev P G, Li B A 2008 Astronphys. J. 685 390 Google Scholar
[33]	Lattimer J M, Schutz B F 2005 Astrophys. J. 629 979 Google Scholar
[34]	Glendenning N K 1997 Compact Stars: Nuclear Physics, Particle Physics, and General Relativity (New York: Springer-Verlag) pp75−78
[35]	Bandyopadhyay D, Chakrabarty S, Pal S 1997 Phys. Rev. Lett. 79 2176 Google Scholar
[36]	Wiringa R B, Fiks V, Fabroeini A 1988 Phys. Rev. 38 1010 Google Scholar
[37]	Manchester R N 2004 Science 304 542 Google Scholar
[38]	Gao Z F, Shan H, Wang H 2021 Astron. Nachr. 342 369 Google Scholar
[39]	Krotscheck E, Kundt W 1978 Commun. Math. Phys. 60 171 Google Scholar
[40]	Demorest P B, Pennucci T, Ransom S M 2010 Nature 467 1081 Google Scholar
[41]	Fonseca E, Pennucci T T, Ellis J A 2016 Astrophys. J. 832 167 Google Scholar
[42]	Antoniadis J, Freire, P C C, Wex N 2013 Science 340 448 Google Scholar
[43]	Cromartie H T, Fonseca E, Ransom S M 2020 Nat. Astron. 4 72 Google Scholar
[44]	Kandel D, Romani R W 2020 Astrophys. J. 892 101 Google Scholar
[45]	Godzieba D A, Radice D, Bernuzzi S 2021 Astrophys. J. 908 122 Google Scholar
[46]	Fattoyev F J, Horowitz C J, Piekarewicz J 2020 Phys. Rev. C 102 065805 Google Scholar
[47]	Liang E P 1986 Astrophys. J. 304 682 Google Scholar

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