论文标题
高度磁化的脉冲星PSR J1846-0258的X射线光谱，其风星云和托管超新星残留KES 75
X-ray Spectroscopy of the Highly Magnetized Pulsar PSR J1846-0258, its Wind Nebula and Hosting Supernova Remnant Kes 75
论文作者
论文摘要
我们介绍了构成超新星残留（SNR）kesteven 75 75的宽带X射线光谱，并使用并发2017年8月17日至20日XMM-NEWTON和NUSTAR观察结果，在此期间发现PULSAR PSR PSR J1846-0258在此期间处于Quiescent Centent状态。年轻的残留物具有由高度能量（EDOT = 8.1E36 ERG/s）驱动的明亮的脉冲星星云，分离出旋转式脉冲星，仅p/2pdot 〜728年的旋转年龄。其推断的磁场（BS = 4.9E13 g）是这些物体已知的最大的磁场，并且可能是导致耀斑和爆发活动间隔的原因，这表明/向磁体状态之间的过渡。 PSR J1846-0258的脉冲发射通过具有光子指数gamma_psr = 1.24 +/- 0.09和2-10 keV Unabsorbed Flux（2.3 +/- 0.4）E-0.4）E-02 ERG/S/s/cm^2的脉冲模型在2-50 keV范围内进行了充分的特征。我们没有发现在当前状态下10 keV以上的其他非热成分的证据，这对于磁场来说是典型的。与Chandra Pulsar光谱相比，在2-10 KEV频段中，固有的脉冲分数为71 +/- 16％。 PWN的幂律频谱在1-55 keV频段中得出γ_pWn= 2.03 +/- 0.03，在此范围内没有曲率的证据，还有2-10 KEV UNABSORBED FLUX（2.13 +/- 0.02）E-01 ERG/S/S/CM^2。 Nustar数据揭示了在10 keV上方的SNR光谱中占主导地位的硬X射线成分的证据，我们将其归因于粉尘散发的PWN分量。我们对KES 75系统的动力学和辐射演化进行建模，以估计中子星的出生特性，其祖细胞的能量和PWN的性质。这表明KES 75的祖先最初是在二进制系统中，该系统将大部分质量转移到伴侣之前。
We present broad-band X-ray spectroscopy of the energetic components that make up the supernova remnant (SNR) Kesteven 75 using concurrent 2017 Aug 17-20 XMM-Newton and NuSTAR observations, during which the pulsar PSR J1846-0258 is found to be in the quiescent state. The young remnant hosts a bright pulsar wind nebula powered by the highly-energetic (Edot = 8.1E36 erg/s) isolated, rotation-powered pulsar, with a spin-down age of only P/2Pdot ~ 728 yr. Its inferred magnetic field (Bs = 4.9E13 G) is the largest known for these objects, and is likely responsible for intervals of flare and burst activity, suggesting a transition between/to a magnetar state. The pulsed emission from PSR J1846-0258 is well-characterized in the 2-50 keV range by a power-law model with photon index Gamma_PSR = 1.24+/-0.09 and a 2-10 keV unabsorbed flux of (2.3+/-0.4)E-12 erg/s/cm^2). We find no evidence for an additional non-thermal component above 10 keV in the current state, as would be typical for a magnetar. Compared to the Chandra pulsar spectrum, the intrinsic pulsed fraction is 71+/-16% in 2-10 keV band. A power-law spectrum for the PWN yields Gamma_PWN = 2.03+/-0.03 in the 1-55 keV band, with no evidence of curvature in this range, and a 2-10 keV unabsorbed flux (2.13+/-0.02)E-11 erg/s/cm^2. The NuSTAR data reveal evidence for a hard X-ray component dominating the SNR spectrum above 10 keV which we attribute to a dust-scattered PWN component. We model the dynamical and radiative evolution of the Kes 75 system to estimate the birth properties of the neutron star, the energetics of its progenitor, and properties of the PWN. This suggests that the progenitor of Kes 75 was originally in a binary system which transferred most its mass to a companion before exploding.
