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Estimating the Black Hole Spin for the X-Ray Binary MAXI J1820+070

Xueshan ZhaoKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Lijun GouKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Yanting DongKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Y. L. TuoKey Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049, People’s Republic Of ChinaZhenxuan LiaoKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Yufeng LiKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Nan JiaKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]Ye FengKey Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Datun Road 20A, Beijing 100101, People’s Republic of China; [email protected], [email protected]James F. SteinerHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

2021en

ABI

Annotatsiya

Abstract MAXI J1820+070 is a newly discovered black hole X-ray binary, whose dynamical parameters, namely the black hole mass, the inclination angle, and the source distance, have recently been estimated. Insight-HXMT have observed its entire outburst from 2018 March 14. In this work, we attempted to estimate the spin parameter a * , using the continuum-fitting method and applying a fully relativistic thin disk model to the soft-state spectra obtained by Insight-HXMT. It is well known that a * is strongly dependent on three dynamical parameters in this method, and we have examined two sets of parameters. Adopting our preferred parameters: M = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>8.48</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.72</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.79</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> , i = 63° ± 3°, and D = 2.96 ± 0.33 kpc, we found a slowly spinning black hole of a * = 0.14 ± 0.09 (1 σ ), which gives a prograde spin parameter as the majority of other systems show. It is also possible for the black hole to have a retrograde spin (less than 0) if different dynamical parameters are taken.

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DOI: 10.3847/1538-4357/ac07a9

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