通过射电观测探索脉冲星风星云PSR J2030+4415背后的非热物理

IF 5.8 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
J. M. Paredes, P. Benaglia, V. Bosch-Ramon, A. Tej, A. Saha, J. Martí, P. Bordas
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引用次数: 0

摘要

上下文。PSR J2030+4415是一颗伽玛射线脉冲星,其x射线脉冲星风星云沿南北方向拉长。该系统显示了一个突出的x射线灯丝,其方向与星云轴成130°角。为了提高我们对脉冲星风星云中发生的非热过程的理解,我们试图确定射电对应物的可能存在,研究其形态,并获得脉冲星和长丝在射电波长下发射的限制性上限。我们利用升级后的巨型米波射电望远镜(uGMRT)在两个频段对脉冲星PSR J2030+4415及其周围进行了观测,并将结果与其他波长的发现联系起来。我们获得了736和1274兆赫的射电图像,显示脉冲星后面有一个结构,其形态与x射线星云重叠。这个射电结构是x射线脉冲星风星云的对应物。推导出的光谱指数沿此结构呈现出空间变化。在任何探索的无线电频率上都没有脉冲星和灯丝的迹象,但我们获得了限制性的上限。结合射电和x射线观测,并与红外数据一致,提出了一个物理场景的星云和灯丝。我们提出,粒子加速发生在星云尾部,是由于再准直激波的存在,最高能量的粒子通过能量依赖的扩散逐渐逃离它。我们还发现了沿~GeV的x射线灯丝逃逸的粒子能量的下限。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Exploring the non-thermal physics behind the pulsar wind nebula PSR J2030+4415 through radio observations
Context. PSR J2030+4415 is a gamma-ray pulsar with an X-ray pulsar wind nebula elongated along the north-south direction. The system shows a prominent X-ray filament oriented at an angle of 130° to the nebula axis.Aims. To improve our understanding of the non-thermal processes occurring in the pulsar wind nebula, we attempted to determine the possible existence of a radio counterpart, study its morphology, and obtain restrictive upper limits of the pulsar and filament emission at radio wavelengths.Methods. We performed observations of the pulsar PSR J2030+4415 and its surroundings with the upgraded Giant Metrewave Radio Telescope (uGMRT) at two frequency bands, and put the results in context with findings at other wavelengths.Results. We obtained radio images at 736 and 1274 MHz that reveal a structure trailing the pulsar, with a morphology overlapping the X-ray nebula. This radio structure is the radio counterpart of the X-ray pulsar wind nebula. The derived spectral index along this structure shows spatial variation. There are no hints of the pulsar and the filament at any of the explored radio frequencies, but we obtained restrictive upper limits. A physical scenario that combines the radio and the X-ray observations, and consistent with IR data, of the nebula and the filament is presented. We propose that particle acceleration occurs in the nebula tail due to the presence of a re-collimation shock, and the highest energy particles gradually escape from it through energy-dependent diffusion. We also find a lower limit in the energy of the particles escaping along the X-ray filament of ~GeV.
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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