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SNR RXJ1713.7-3946 keV/TeV联合观测， 轻子？强子？

Best observations in TeV----shell-type SNRs give us more know about CRs acceleration----diffusive shock acceleration But electron or hadron?. SNR RXJ1713.7-3946 keV/TeV联合观测， 轻子？强子？. A&A. 449 (2006) 223-242. A&A ， 464(2007)235-243. 距离： 1 kpc 年龄： 1600 年 半径： 1 度 流强（ 1TeV ）： 70%Crab.

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SNR RXJ1713.7-3946 keV/TeV联合观测， 轻子？强子？

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  1. Best observations in TeV----shell-type SNRsgive us more know about CRs acceleration----diffusive shock accelerationBut electron or hadron?

  2. SNR RXJ1713.7-3946 keV/TeV联合观测，轻子？强子？ A&A. 449 (2006) 223-242 A&A，464(2007)235-243 距离：1 kpc 年龄：1600 年 半径：1度 流强（1TeV）：70%Crab 轻子模型 强子模型

  3. SNR RXJ1713.7-3946 keV/TeV联合观测，+GeV观测，偏向于强子？ A&A. 449 (2006) 223-242 A&A，464(2007)235-243 距离：1 kpc 年龄：1600 年 半径：1度 流强（1TeV）：70%Crab 轻子模型 强子模型 Fermi 初步结果

  4. New anisotropy component and corotation evidence of the GCR (Science 314(2006)439-443) Celestial Intensity map (E~3TeV) Intensity @ E~300TeV New anisotropy component Amp=0.16% w/o corotation; Observation: 0.03%±0.03%.

  5. All-particle spectrum measured by Tibet-III array(ApJ 678, 1165-1179 (2008)) A sharp knee around 4 PeV is clearly seen. 6 Jing Huang (ISVH2008-PARIS)

  6. 10° 0° -10° 180° 0° 120° 60° 240° 180° 300° Diffuse Gamma Rays from Galactic Plane Electron model Electron model p0 model p0 model EGRET data

  7. 已有的多波段观测+100TeV γ射线观测有助于确定宇宙线强子源 A&A，464(2007)235-243 100TeVγ射线的观测极大地增强了我们对宇宙线强子源的认识， 距离：1 kpc 年龄：1600 年 半径：1度 流强（1TeV）：70%Crab SNR RXJ1713.7-3946 强子模型

  8. Background and signal

  9. 超出 LHC的 千万倍！ 宇宙线的成份和能谱 • 主要是原子核：P，He，…, Fe,… • 也有：，e± • 还有：γ，ν • 最高宇宙线粒子的能量达到3×1020eV，约50焦耳。从那里，又是如何被加速到这样的能量还是一个未解的迷 • 宇宙线电子，伽玛射线，中微子对宇宙线起源，加速，对暗物质寻找，对量子引力研究有重要意义。

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