Philip Kaaret, Oliver J. Roberts, Steven R. Ehlert, Douglas A. Swartz, Martin C. Weisskopf, Ioannis Liodakis, M. Lynne Saade, Stephen L. O’Dell and Chien-Ting Chen
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引用次数: 0
摘要
一些 X 射线双星包含一颗围绕正常恒星运行的高能脉冲星，在脉冲星和恒星风碰撞形成的冲击锥中，粒子加速到高能量。这类双星加速区域的磁场几何形状尚不清楚。我们首次测量了伽马射线双星系统发出的X射线同步辐射的偏振。我们利用成像 X 射线偏振探测仪观测了 PSR B1259-63，观测期间正值 2024 年 6 月近地点穿越后的 X 射线明亮阶段。探测到的 X 射线偏振的偏振度为 8.3% ± 1.5%，显著性为 5.3σ。X 射线偏振角与观测时的冲击锥轴线一致。这表明加速区磁场的主要分量垂直于冲击锥轴线。
Magnetic Field Geometry of the Gamma-Ray Binary PSR B1259–63 Revealed via X-Ray Polarization
Some X-ray binaries containing an energetic pulsar in orbit around a normal star accelerate particles to high energies in the shock cone formed where the pulsar and stellar winds collide. The magnetic field geometry in the acceleration region in such binaries is unknown. We performed the first measurement of the polarization of the X-ray synchrotron emission from a gamma-ray-emitting binary system. We observed PSR B1259–63 with the Imaging X-ray Polarimetry Explorer during an X-ray bright phase following the periastron passage in 2024 June. X-ray polarization is detected with a polarization degree of 8.3% ± 1.5% at a significance of 5.3σ. The X-ray polarization angle is aligned with the axis of the shock cone at the time of the observation. This indicates that the predominant component of the magnetic field in the acceleration region is oriented perpendicular to the shock-cone axis.
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