Probing The Radio To X-ray Connection Of The Vela X Pulsar Wind Nebula With Fermi Lat And H.e.s.s.

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  《The Astrophysical journal》 |2008年第2apart2期|125-128|共4页
• 作者

  O. C. de Jager; P. O. Slane; S. LaMassa;

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  morphologically; it appears as if the vela x pulsar wind nebula (pwn) consists of two emission regions: whereas x-ray (～1 kev) and very high energy (vhe) h.e.s.s. γ-ray observations appear to define a cocoon-type shape south of the pulsar; radio observations reveal an extended area of size 2° × 3° (including the cocoon area); also south of the vela pulsar. since no wide field of view (fov) observations of the synchrotron emission between radio and x-rays are available; we do not know how the lepton (e~±) spectra of these two components connect or how the morphology changes with energy. currently; we find that two distinct lepton spectra describe the respective radio and x-ray/vhe γ-ray spectra; with a field strength of 5 μg self-consistently describing a radiation spectral break (or energy maxim;

  机译：从形态上看;似乎vela x脉冲星风星云（pwn）由两个发射区域组成：而x射线（〜1 kev）和非常高的能量（vhe）h.s.s. γ射线观测似乎在脉冲星以南定义了茧型形状;无线电观测显示了大小为2°×3°的扩展区域（包括茧形区域）;也在韦拉脉冲星以南。由于没有关于无线电和X射线之间的同步加速器发射的宽视场（fov）观测;我们不知道这两个分量的轻子（e〜±）光谱如何连接或形态如何随能量变化。目前;我们发现两个不同的轻子光谱分别描述了无线电和x射线/ vheγ射线光谱;5μg的场强自洽地描述了辐射光谱破裂（或能量最大值）;