Discovery of hard nonthermal pulsed X-ray emission from the anomalous X-ray pulsar 1E 1841-045
Discovery of hard nonthermal pulsed X-ray emission from the anomalous X-ray pulsar 1E 1841-045
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DOI：
10.1086/423129
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发表时间：
2004-10-01
影响因子：
4.9
通讯作者：
Mendez, M
中科院分区：
文献类型：
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作者：
Kuiper, L;Hermsen, W;Mendez, M
我们报告使用罗西 X 射线计时探测器 (RXTE) 比例计数器阵列和高能 X 射线计时实验 (HEXTE) 数据，发现位于超新星遗迹 Kes 73 中心附近的异常 11.8 s X 射线脉冲星 AXP 1E 1841 - 045 发射高达 150 keV 的非热脉冲 X 射线/软伽马射线。双峰脉冲轮廓的形态随着能量从 2 keV 到大约 8 keV 快速变化，高于该能量，脉冲形状或多或少保持稳定。脉冲频谱很硬；其在 10 keV 以上的形状可以通过光子指数为 0.94 +/- 0.16 的幂律来很好地描述。 1E 1841 - 045 是第一个检测到如此强脉冲发射的 AXP，它指向磁星磁层的起源。我们还使用 RXTE HEXTE 和 XMM-Newton pn 数据从 Kes 73/1E 1841 - 045 复合体导出了类似 1 - 270 keV 能量范围的总发射光谱。将复合体的总发射与来自 Chandra ACIS CC 模式数据（Morii 等人，2003）的 1E 1841 - 045 的脉冲+DC 发射进行比较，为 Kes 73 在接近 7 keV 或更高能量下的发射留下了很小的空间。这表明上面类似于 15 keV 的 HEXTE 谱，由指数 1.47 +/- 0.05 的幂律令人满意地描述，主要由 1E 1841 - 045 的发射主导。在这种情况下，10 keV 以上能量的脉冲分数将从 10 keV 附近的约 25% 增加到 100 keV 附近的 100%。延伸至大约 100 keV 的直流分量的起源可能是磁层，并且可能是所有相位“开启”的脉冲发射的表现。
We report the discovery of nonthermal pulsed X-ray/soft gamma-ray emission up to similar to 150 keV from the anomalous 11.8 s X-ray pulsar AXP 1E 1841 - 045 located near the center of supernova remnant Kes 73 using Rossi X-Ray Timing Explorer (RXTE) Proportional Counter Array and High Energy X-Ray Timing Experiment (HEXTE) data. The morphology of the double-peaked pulse profile changes rapidly with energy from 2 keV up to similar to 8 keV, above which the pulse shape remains more or less stable. The pulsed spectrum is very hard; its shape above 10 keV can be described well by a power law with a photon index of 0.94 +/- 0.16. 1E 1841 - 045 is the first AXP for which such very hard pulsed emission has been detected, which points to an origin in the magnetosphere of a magnetar. We have also derived the total emission spectrum from the Kes 73/1E 1841 - 045 complex for the similar to1 - 270 keV energy range using RXTE HEXTE and XMM-Newton pn data. A comparison of the total emission from the complex with the pulsed+DC emission from 1E 1841 - 045 as derived from Chandra ACIS CC-mode data (Morii et al. 2003) leaves little room for emission from Kes 73 at energies near 7 keV or above. This suggests that the HEXTE spectrum above similar to 15 keV, satisfactorily described by a power law with index 1.47 +/- 0.05, is dominated by emission from 1E 1841 - 045. In that case the pulsed fraction for energies above 10 keV would increase from about 25% near 10 keV to 100% near 100 keV. The origin of the DC-component extending up to similar to 100 keV is probably magnetospheric and could be a manifestation of pulsed emission that is "on'' for all phases.