arXiv 0706.05062007-06-05astro-ph

在Cosmic-Ray相互作用中产生的漫射γ射线和RX的TeV-band光谱J1713. 7 -3946

Diffuse Gamma-Rays Produced in Cosmic-Ray Interactions and the TeV-band Spectrum of RX J1713.7-3946

C. -Y. Huang, M. Pohl, S. -E. Park, C. D. Daniels

备注：: 4 pages; 5 figures; Contribution to the 30th ICRC, Merida, Mexico, 2007; References included

摘要：

我们采用蒙特卡罗粒子碰撞程序DPMJET 3.04计算了宇宙射线（$p$和$α$）与星际介质相互作用中产生的以$γ$为最终衰变态的各种次级粒子（除$π^0$外）的多重数谱。我们推导出一个易于使用的$γ$ -射线生产矩阵的宇宙射线能量高达约10 PeV。这个$γ$射线产生矩阵被应用于EGRET观测到的银河系弥散$γ$射线中的GeV过量，我们得出结论，非$π^0$衰变成分不足以解释GeV过量，尽管它们贡献了与$π^0$衰变成分不同的光谱。我们还检验了这样的假设：用HESS观察到的壳型SNR RX J1713.7-3946的TeV波段$γ$射线发射是由强子宇宙线引起的，这些宇宙线被宇宙线修改冲击加速。通过$χ^2$统计，我们发现一个连续软化的光谱是强烈的首选，与预期相反。一个硬化谱有大约1%的概率来解释HESS数据，但只有当一个硬截止在50-100 TeV的粒子谱。

英文摘要：

We employ the Monte Carlo particle collision code DPMJET3.04 to determine the multiplicity spectra of various secondary particles (in addition to $π^0$'s) with $γ$'s as the final decay state, that are produced in cosmic-ray ($p$'s and $α$'s) interactions with the interstellar medium. We derive an easy-to-use $γ$-ray production matrix for cosmic rays with energies up to about 10 PeV. This $γ$-ray production matrix is applied to the GeV excess in diffuse Galactic $γ$-rays observed by EGRET, and we conclude the non-$π^0$ decay components are insufficient to explain the GeV excess, although they have contributed a different spectrum from the $π^0$-decay component. We also test the hypothesis that the TeV-band $γ$-ray emission of the shell-type SNR RX J1713.7-3946 observed with HESS is caused by hadronic cosmic rays which are accelerated by a cosmic-ray modified shock. By the $χ^2$ statistics, we find a continuously softening spectrum is strongly preferred, in contrast to expectations. A hardening spectrum has about 1% probability to explain the HESS data, but then only if a hard cutoff at 50-100 TeV is imposed on the particle spectrum.

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