Relation of Cyclotron Resonant Energy and Luminosity in a Strongly Magnetized Neutron Star GRO J1008-57 Observed by Insight-HXMT
Relation of Cyclotron Resonant Energy and Luminosity in a Strongly Magnetized Neutron Star GRO J1008-57 Observed by Insight-HXMT
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Insight-HXMT观测的强磁化中子星GRO J1008-57回旋共振能量与光度关系
DOI：
10.3847/1538-4357/ac1268
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发表时间：
2021-07
期刊：
影响因子：
--
通讯作者：
et al.
中科院分区：
文献类型：
--
作者：
Chen X.;Wang W.;Tang Y. M.;et al.
回旋线散射特征在几十个X射线衍射仪（XRP）中被检测到，并被用作吸积中子星（NS）表面强磁场的直接指示器。在少数情况下，回旋线是已知的XRP吸积光度的变量。人们接受的是，所观察到的回旋线散射功能的变化有关的NS的磁极上方的吸积流的几何形状和动力学的变化。线质心能量和光度之间的正相关性对于亚临界XRP是典型的，其中吸积导致磁极处的热点。负相关性被认为是明亮的超临界XRP的一个特定特征，其中辐射压力支持恒星表面上方的吸积柱。在Be瞬态XRP GRO J1008-57的光谱中的回旋线被检测到的能量从1.75到90 keV，在XRP中回旋线特征的最高观测能量。本文报道了2017年8月由Insight-HXMT观测到的GRO J1008-57 II型爆发中回旋线质心能量与光度的特殊关系。回旋线能量在3.2 × 1037 erg s−1 < L < 4.2 × 1037 erg s−1时与光度呈负相关，在L <5 × 1037 erg s−1时与光度呈正相关。我们推测，所观察到的回旋加速器线的特殊行为将是由于吸积通道几何形状的变化。
Cyclotron line scattering features are detected in a few tens of X-ray pulsars (XRPs) and used as direct indicators of a strong magnetic field at the surface of accreting neutron stars (NSs). In a few cases, cyclotron lines are known to be variable with the accretion luminosity of XRPs. It is accepted that the observed variations of cyclotron line scattering features are related to variations of geometry and dynamics of accretion flow above the magnetic poles of an NS. A positive correlation between the line centroid energy and luminosity is typical for subcritical XRPs, where the accretion results in hot spots at the magnetic poles. The negative correlation was proposed to be a specific feature of bright supercritical XRPs, where radiation pressure supports accretion columns above the stellar surface. The cyclotron line in the spectra of the Be-transient XRP GRO J1008-57 is detected at energies from ∼75 to 90 keV, the highest observed energy of a cyclotron line feature in XRPs. We report the peculiar relation of cyclotron line centroid energies with luminosity in GRO J1008-57 during the Type II outburst in 2017 August observed by Insight-HXMT. The cyclotron line energy was detected to be negatively correlated with the luminosity at 3.2 × 1037 erg s−1 < L < 4.2 × 1037 erg s−1 and positively correlated at L ≳ 5 × 1037 erg s−1. We speculate that the observed peculiar behavior of a cyclotron line would be due to variations of accretion channel geometry.
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DOI：
10.1007/s00159-015-0082-6
发表时间：
2013-05
期刊：
The Astronomy and Astrophysics Review
影响因子：
--
作者：
R. Walter;A. Lutovinov;E. Bozzo;S. Tsygankov
通讯作者：
R. Walter;A. Lutovinov;E. Bozzo;S. Tsygankov
DOI：
10.1134/s1063773707060023
发表时间：
2007-04
期刊：
Astronomy Letters
影响因子：
--
作者：
S. Tsygankov;A. Lutovinov;E. Churazov;R. S. R. Institute-R.-S.-R.-Institute-102350741;Moscow;Russia Mpi for Astrophysik;Garching;Germany
通讯作者：
S. Tsygankov;A. Lutovinov;E. Churazov;R. S. R. Institute-R.-S.-R.-Institute-102350741;Moscow;Russia Mpi for Astrophysik;Garching;Germany
DOI：
10.1111/j.1365-2966.2009.15791.x
发表时间：
2009-09
影响因子：
4.8
作者：
S. Tsygankov;A. Lutovinov;A. L. M. F. Astrophysics;Garching;H Germany;S. R. Institute;Moscow;Russia.;I. Physics;N. Novgorod
通讯作者：
S. Tsygankov;A. Lutovinov;A. L. M. F. Astrophysics;Garching;H Germany;S. R. Institute;Moscow;Russia.;I. Physics;N. Novgorod
DOI：
10.1088/0004-637x/780/2/133
发表时间：
2013-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. Fuerst;K. Pottschmidt;J. Wilms;J. Tomsick;M. Bachetti;S. Boggs;F. Christensen;W. Craig;B. Grefenstette;C. Hailey;F. Harrison;K. Madsen;Jonathan M. Miller;D. Stern;D. Walton;Will Zhang
通讯作者：
F. Fuerst;K. Pottschmidt;J. Wilms;J. Tomsick;M. Bachetti;S. Boggs;F. Christensen;W. Craig;B. Grefenstette;C. Hailey;F. Harrison;K. Madsen;Jonathan M. Miller;D. Stern;D. Walton;Will Zhang
DOI：
10.3847/2041-8213/ab3e4d
发表时间：
2019-09
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
S. Molkov;A. Lutovinov;S. Tsygankov;I. Mereminskiy;A. Mushtukov
通讯作者：
S. Molkov;A. Lutovinov;S. Tsygankov;I. Mereminskiy;A. Mushtukov