NuSTAR DISCOVERY OF AN UNUSUALLY STEADY LONG-TERM SPIN-UP OF THE Be BINARY 2RXP J130159.6–635806
NuSTAR DISCOVERY OF AN UNUSUALLY STEADY LONG-TERM SPIN-UP OF THE Be BINARY 2RXP J130159.6–635806
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DOI：
10.1088/0004-637x/809/2/140
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发表时间：
2015-07
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通讯作者：
R. Krivonos;S. Tsygankov;A. Lutovinov;J. Tomsick;D. Chakrabarty;M. Bachetti;S. Boggs;M. Chernyakova;F. Christensen;W. Craig;F. Fuerst;C. Hailey;F. Harrison;G. Lansbury;F. Rahoui;D. Stern;W. L. H. U. Berkeley;Ca;Usa;S. R. Institute;R. A. O. Sciences;Moscow;Russia.;T. Observatory;D. Physics;Astronomy;U. Turku;Finland.;Mit Kavli Institute for Astrophysics;S. Research;Cambridge;Ma;O. Midi-Pyrenees;U. Toulouse;France.;Cnrs;Institut de Recherche en Astrophysique et Planetologie-Institut-de-Recherche-en-Astrophysique-et-102437653;Toulouse;Dublin City University;Ireland;Dublin Institute for Advanced Studies;D. S. -. N. S. Institute-D.-S.-.-N.-S.-Institute-1388847304;T. Denmark;Denmark;Lawrence Livermore National Laboratory;Livermore;C. 9. Astronomy;Astrophysics;C. I. O. Technology.;Pasadena;Columbia Astrophysics Laboratory;C. University;New York.;U. Durham;UK.;E. Observatory;G. B. Muenchen;H Germany;D. O. Astronomy;Harvard University;Jet propulsion Laboratory;Nasa Goddard Space Flight Center;Greenbelt;Md
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作者：
R. Krivonos;S. Tsygankov;A. Lutovinov;J. Tomsick;D. Chakrabarty;M. Bachetti;S. Boggs;M. Chernyakova;F. Christensen;W. Craig;F. Fuerst;C. Hailey;F. Harrison;G. Lansbury;F. Rahoui;D. Stern;W. L. H. U. Berkeley;Ca;Usa;S. R. Institute;R. A. O. Sciences;Moscow;Russia.;T. Observatory;D. Physics;Astronomy;U. Turku;Finland.;Mit Kavli Institute for Astrophysics;S. Research;Cambridge;Ma;O. Midi-Pyrenees;U. Toulouse;France.;Cnrs;Institut de Recherche en Astrophysique et Planetologie-Institut-de-Recherche-en-Astrophysique-et-102437653;Toulouse;Dublin City University;Ireland;Dublin Institute for Advanced Studies;D. S. -. N. S. Institute-D.-S.-.-N.-S.-Institute-1388847304;T. Denmark;Denmark;Lawrence Livermore National Laboratory;Livermore;C. 9. Astronomy;Astrophysics;C. I. O. Technology.;Pasadena;Columbia Astrophysics Laboratory;C. University;New York.;U. Durham;UK.;E. Observatory;G. B. Muenchen;H Germany;D. O. Astronomy;Harvard University;Jet propulsion Laboratory;Nasa Goddard Space Flight Center;Greenbelt;Md
我们对吸积 X 射线脉冲星 2RXP J130159.6–635806 的核光谱望远镜阵列 (NuSTAR) 观测结果进行了光谱和定时分析。该源是在一次针对伽马射线双星 PSR B1259-63 的活动中偶然观测到的，后来被定为专门观测的目标。光谱具有吸积 X 射线脉冲星的典型形状，由简单的幂律组成，指数截止起始于 ∼7 keV，折叠能量为 E 折叠 ≃ 18 ?> keV。还表明光谱中存在~3 ?> 显着性水平的 6.4 keV 铁谱线。 NuSTAR 对脉动周期的测量表明，脉冲星在过去 20 年里经历了强劲而稳定的自转。脉冲分数估计为 ∼ 80 % ?> ，并且在能量高达 40 keV 时保持恒定。功率密度谱显示相对于当前旋转周期向更高频率的突破。这与稳定持续的光度一起表明，长期质量吸积率足够高，足以使脉冲星脱离自旋平衡。
We present spectral and timing analyses of Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the accreting X-ray pulsar 2RXP J130159.6–635806. The source was serendipitously observed during a campaign focused on the gamma-ray binary PSR B1259–63 and was later targeted for a dedicated observation. The spectrum has a typical shape for accreting X-ray pulsars, consisting of a simple power law with an exponential cutoff starting at ∼7 keV with a folding energy of E fold ≃ 18 ?> keV. There is also an indication of the presence of a 6.4 keV iron line in the spectrum at the ∼ 3 ?> significance level. NuSTAR measurements of the pulsation period reveal that the pulsar has undergone a strong and steady spin-up for the last 20 years. The pulsed fraction is estimated to be ∼ 80 % ?> , and is constant with energy up to 40 keV. The power density spectrum shows a break toward higher frequencies relative to the current spin period. This, together with steady persistent luminosity, points to a long-term mass accretion rate high enough to bring the pulsar out of spin equilibrium.