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arXiv 0810.0094astro-ph
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SNR RX J1713 .7-3946的Gamma ray发射和银河系宇宙射线的起源

Gamma ray emission from SNR RX J1713.7-3946 and the origin of galactic cosmic rays

G. Morlino, E. Amato, P. Blasi

备注：
Accepted for Publication in MNRAS
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摘要：

我们计算的非热辐射的流量从超新星遗迹RX J1713.7-3946的背景下，在冲击波的粒子加速的非线性理论，这使我们能够考虑自洽的动力学反应的加速粒子，产生的磁场在冲击波附近和等离子体上的动态反应的磁场。当得到加速的粒子的分数是$\sim 10^{-4}$阶，我们发现，作为由宇宙射线引起的流不稳定性的结果获得的磁场的强度是兼容的X射线发射灯丝的解释产生的强同步辐射损失在$\sim 100 μG$磁场。如果以替代方式解释X射线细丝，则对激波下游的磁场的约束消失，并且HESS数据可以与复杂光子群的相对论电子的ICS略微拟合，该光子群被定制为包括CMB和环境IR/光学光子。这种拟合在最高能量时通常很差，需要在残余物内有大密度的目标光子;只有一小部分$\sim 10^{-6}$阶的背景粒子得到加速;局部磁场是$\sim 20μG$阶的，质子的最大能量远低于膝能。目前的HESS伽马射线观测结合朱雀最近的X射线观测，还不能得出RX J1713.7-3946是否是一个有效的宇宙射线加速器的明确结论，尽管目前HESS数据的强子解释似乎更有可能。我们讨论了GLAST伽马射线望远镜，这应该能够区分上述两种情况下，我们的结果的影响。

英文摘要：

We calculate the flux of non-thermal radiations from the supernova remnant RX J1713.7-3946 in the context of the non-linear theory of particle acceleration at shocks, which allows us to take into account self-consistently the dynamical reaction of the accelerated particles, the generation of magnetic fields in the shock proximity and the dynamical reaction of the magnetic field on the plasma. When the fraction of particles which get accelerated is of order $\sim 10^{-4}$, we find that the strength of the magnetic field obtained as a result of streaming instability induced by cosmic rays is compatible with the interpretation of the X-ray emitting filaments being produced by strong synchrotron losses in $\sim 100 μG$ magnetic fields. If the X-ray filaments are explained in alternative ways, the constraint on the magnetic field downstream of the shock disappears and the HESS data can be marginally fit with ICS of relativistic electrons off a complex population of photons, tailored to comprise CMB and ambient IR/Optical photons. The fit, typically poor at the highest energies, requires a large density of target photons within the remnant; only a fraction of order $\sim 10^{-6}$ of the background particles gets accelerated; the local magnetic field is of order $\sim 20μG$ and the maximum energy of protons is much lower than the knee energy. Current HESS gamma ray observations combined with recent X-ray observations by Suzaku do not allow as yet to draw a definitive conclusion on whether RX J1713.7-3946 is an efficient cosmic ray accelerator, although at the present time a hadronic interpretation of HESS data seems more likely. We discuss the implications of our results for the GLAST gamma ray telescope, which should be able to discriminate the two scenarios discussed above.

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