Could very high energy gamma rays from the crab nebula result from p-p collision?
Could very high energy gamma rays from the crab nebula result from p-p collision?
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DOI：
10.1088/0954-3899/16/7/022
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发表时间：
1990-07
期刊：
影响因子：
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通讯作者：
K. Cheng;T. Cheung;M. Lau;K. N. Yu;P. Kwok
中科院分区：
文献类型：
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作者：
K. Cheng;T. Cheung;M. Lau;K. N. Yu;P. Kwok
一般认为，蟹状星云发射的甚高能量（VHE）伽马射线不可能是由中性π介子衰变产生的，而中性π介子是由相对论质子碰撞产生的，因为星云的强子截面很小，柱密度也很低。然而，蟹状星云的磁场可以捕获来自脉冲星的大量相对论质子，总能量高达1047 erg，因为同样的原因，这些能量很难释放。然而，少量的质子将通过偶然的强子碰撞转换为VHE光子，这导致稳定的VHE伽马射线发射，平均功率约为4 * 1034 erg s-1。利用Ruderman和Cheng（1988）提出的脉冲星演化模型计算了质子能谱。
It is generally believed that the very high energy (VHE) gamma rays emitted from the Crab Nebula cannot result from the decay of neutral pions which are produced by the collision between relativistic protons, due to the small hadronic cross section and low column density of the nebula. However, the magnetic field of the Crab Nebula could trap a large amount of relativistic protons from the pulsar with a total energy of up to 1047 erg, because this amount of energy is difficult to release for the same reason. Nevertheless, a small amount of protons will be converted to VHE photons through occasional hadronic collisions which result in steady VHE gamma ray emission with an average power of approximately 4*1034 erg s-1. The authors calculate the proton energy spectrum by using the pulsar evolution model proposed by Ruderman and Cheng (1988).