在本论文中，我们首先简要介绍了脉冲星及脉冲星风云的基本知识，包括脉冲星风云 的基本理论及观测进展。在此基础上，我们研究了Crab星云多波段非热辐射。一般认为，星风云中的 相对论电子有两种成份：一种直接来自脉冲星磁层，另一种来自星风云中的激波加速， 相对论性电子的分布满足一折断的幂律谱。我们考虑了相对论电子随时间的演化情况，计算了 其产生的同步辐射和逆康普顿散射能谱。相对论性电子的同步辐射产生了Crab星云所观测到的 从射电到中能伽玛射线的辐射，而这些电子与同步辐射光子、星际红外光子和宇宙微波背景辐射 光子之间的逆康普顿散射产生了所观测到的伽玛射线辐射。我们的理论预言与观测结果吻合很好。; In this thesis，we study the multi-band radiation from Crab Nebula. We first introduce the theory about pulsar wind nebulae (PWNe), which include the recent observation and the evolution. Generally, the relativistic electrons in the PWNe consist of two components, one comes directly from pulsar magnetosphere, another from the shock acceleration in the PWNe. So the distribution of the electrons is a broken power law with different indices and a break energy. Based on a simplified time-dependent injection model of the relativistic electrons, we give out the energy spectrum of the Crab nebula from radio to TeV gamma-ray bands. In this model, primarily accelerated electrons are injected temporally into the nebula. The accelerated electrons emit nonthermal photons through synchrotron radiation and inverse Compton scattering off soft photon fields. The emission from radio to medium gamma-rays is from electron's synchrotron radiation, whereas the high-energy photons primarily come from the inverse Compton scattering of the relativistic electrons on synchrotron photons. The resulting spectrum calculated is well consistent with the observed data ranging from radio to VHE gamma-rays for the Crab nebula.
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