Accretion torque reversals in GRO J1008-57 revealed by Insight-HXMT

被引：73

作者：

Wang, W. ^{[1
,2
]}

Tang, Y. M. ^{[1
,2
]}

Tuo, Y. L. ^{[3
,4
]}

Epili, P. R. ^{[1
,2
]}

Zhang, S. N. ^{[3
,4
]}

Song, L. M. ^{[3
]}

Lu, F. J. ^{[3
]}

Qu, J. L. ^{[3
]}

Zhang, S. ^{[3
]}

Ge, M. Y. ^{[3
]}

Huang, Y. ^{[3
]}

Li, B. ^{[3
]}

Bu, Q. C. ^{[3
]}

Cai, C. ^{[3
]}

Cao, X. L. ^{[3
]}

Chang, Z. ^{[3
]}

Chen, L. ^{[5
]}

Chen, T. X. ^{[3
]}

Chen, Y. B. ^{[6
]}

Chen, Y. ^{[3
]}

Chen, Y. P. ^{[3
]}

Cui, W. W. ^{[3
]}

Du, Y. Y. ^{[3
]}

Gao, G. H. ^{[3
,4
]}

Gao, H. ^{[3
,4
]}

Gu, Y. D. ^{[3
]}

Guan, J. ^{[3
]}

Guo, C. C. ^{[3
,4
]}

Han, D. W. ^{[3
]}

Huo, J. ^{[3
]}

Jia, S. M. ^{[3
]}

Jiang, W. C. ^{[3
]}

Jin, J. ^{[3
]}

Kong, L. D. ^{[3
,4
]}

Li, C. K. ^{[3
]}

Li, G. ^{[3
]}

Li, T. P. ^{[3
,4
,7
]}

Li, W. ^{[3
]}

Li, X. ^{[3
]}

Li, X. B. ^{[3
]}

Li, X. F. ^{[3
]}

Li, Z. W. ^{[3
]}

Liang, X. H. ^{[3
]}

Liao, J. Y. ^{[3
]}

Liu, B. S. ^{[3
]}

Liu, C. Z. ^{[3
]}

Liu, H. X. ^{[3
]}

Liu, H. W. ^{[3
]}

Lu, X. F. ^{[3
]}

Luo, Q. ^{[3
,4
]}

机构：

[1] Wuhan Univ, Sch Phys & Technol, Wuhan 430072, Peoples R China

[2] Wuhan Univ, WHU NAOC Joint Ctr Astron, Wuhan 430072, Peoples R China

[3] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China

[4] Chinese Acad Sci, Univ Chinese Acad Sci, Beijing 100049, Peoples R China

[5] Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China

[6] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China

[7] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China

[8] Chinese Acad Sci, Inst High Energy Phys, Comp Div, Beijing 100049, Peoples R China

[9] Hebei Univ, Coll Phys Sci & Technol, Baoding 071002, Hebei, Peoples R China

[10] Xiangtan Univ, Sch Phys & Optoelect, Xiangtan 411105, Hunan, Peoples R China

来源：

JOURNAL OF HIGH ENERGY ASTROPHYSICS | 2021年 / 30卷

关键词：

Accretion; Accretion disk; Pulsars: general; Pulsars: individual (GRO J1008-57); QUASI-PERIODIC OSCILLATIONS; NEUTRON-STARS; FASTNESS PARAMETER; CYCLOTRON LINE; GIANT OUTBURST; FIRM DETECTION; 4U 0115+63; ENERGY; DISCOVERY; SPECTRUM;

D O I：

10.1016/j.jheap.2021.01.002

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GRO J1008-57, as a Be/X-ray transient pulsar, is considered to have the highest magnetic field in known neutron star X-ray binary systems. Observational data of the X-ray outbursts in GRO J1008-57 from 2017 to 2020 were collected by the Insight-HXMT satellite. In this work, the spin period of the neutron star in GRO J1008-57 was determined to be about 93.28 seconds in August 2017, 93.22 seconds in February 2018, 93.25 seconds in June 2019 and 93.14 seconds in June 2020. GRO J1008-57 evolved in the spin-up process with a mean rate of -(2.10 +/- 0.05)x10(-4) s/d from 2009 - 2018, and turned into a spin down process with a rate of (6.7 +/- 0.6)x10(-5) s/d from Feb 2018 to June 2019. During the type II outburst of 2020, GRO J1008-57 had the spin-up torque again. During the torque reversals, the pulse profiles and continuum X-ray spectra did not change significantly, and the cyclotron resonant scattering feature around 80 keV was only detected during the outbursts in 2017 and 2020. Based on the observed mean spin-up rate, we estimated the inner accretion disk radius in GRO J1008-57 (about 1 -2 times of the Alfven radius) by comparing different accretion torque models of magnetic neutron stars. During the spin-down process, the magnetic torque should dominate over the matter accreting inflow torque, and we constrained the surface dipole magnetic field B >= 6 x 10(12) G for the neutron star in GRO J1008-57, which is consistent with the magnetic field strength obtained by cyclotron line centroid energy. (C) 2021 Elsevier B.V. All rights reserved.

引用

页码：1 / 8

页数：8

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