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The nature of the X-ray filaments around bow shock pulsar wind nebulae
Astronomy & Astrophysics ( IF 6.5 ) Pub Date : 2024-03-28 , DOI: 10.1051/0004-6361/202449382 Barbara Olmi , Elena Amato , Rino Bandiera , Pasquale Blasi
Astronomy & Astrophysics ( IF 6.5 ) Pub Date : 2024-03-28 , DOI: 10.1051/0004-6361/202449382 Barbara Olmi , Elena Amato , Rino Bandiera , Pasquale Blasi
Context. We propose that the X-ray filaments emerging from selected bow shock pulsar wind nebulae are due to a charge-separated outflow of electrons and/or positrons escaping the nebula and propagating along the local Galactic magnetic field.Aims. The X-ray brightness, length, and thickness of filaments are all accounted for if a nonresonant streaming instability is excited.Methods. This is possible if particles are released in the interstellar medium as a collimated beam, as would be expected in a reconnection region between the nebular and interstellar magnetic fields.Results. We successfully test this idea on the Guitar Nebula filament and discuss other cases.Conclusions. These filaments provide the best diagnostics available for particle escape from evolved pulsar wind nebulae, a process essential to assessing the contribution of these sources to cosmic ray positrons. The same phenomenology might govern the occurrence of TeV halos and their importance for cosmic ray transport.
中文翻译：
弓形激波脉冲星风星云周围 X 射线细丝的性质
语境。我们认为，从选定的弓形激波脉冲星风星云中出现的 X 射线细丝是由于电子和/或正电子逃离星云并沿着局部银河磁场传播的电荷分离流出所致。目标。如果激发非共振流不稳定性，则需考虑细丝的 X 射线亮度、长度和厚度。方法。如果粒子以准直光束的形式释放到星际介质中，这是可能的，正如在星云和星际磁场之间的重新连接区域中所预期的那样。结果。我们在吉他星云灯丝上成功测试了这个想法，并讨论了其他案例。结论。这些细丝为从演化的脉冲星风星云中逃逸的粒子提供了最佳的诊断方法，这是评估这些源对宇宙射线正电子的贡献所必需的过程。同样的现象可能决定 TeV 晕的出现及其对宇宙射线传输的重要性。
更新日期：2024-03-28
中文翻译：
弓形激波脉冲星风星云周围 X 射线细丝的性质
语境。我们认为，从选定的弓形激波脉冲星风星云中出现的 X 射线细丝是由于电子和/或正电子逃离星云并沿着局部银河磁场传播的电荷分离流出所致。目标。如果激发非共振流不稳定性，则需考虑细丝的 X 射线亮度、长度和厚度。方法。如果粒子以准直光束的形式释放到星际介质中，这是可能的，正如在星云和星际磁场之间的重新连接区域中所预期的那样。结果。我们在吉他星云灯丝上成功测试了这个想法，并讨论了其他案例。结论。这些细丝为从演化的脉冲星风星云中逃逸的粒子提供了最佳的诊断方法，这是评估这些源对宇宙射线正电子的贡献所必需的过程。同样的现象可能决定 TeV 晕的出现及其对宇宙射线传输的重要性。
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