In high energy astrophysics scenarios such as blazars, GRBs or PWNe, it is highly probable that ultra-relativistic particles interact with photons in their environment through scattering. As long as the energy of the particle is greater than the energy of the interacting photon, the (classical) scattering is known to be in the Thomson regime. Otherwise, quantum effects will affect the scattering cross section, and we enter into the so-called Klein-Nishina regime. It is well known that radiative cooling in the Thomson regime is very efficient, leading to soft high-energy spectra. However, observations have shown that, in many cases, the high energy spectrum of some objects is rather hard. This has led to think that maybe particles are not being cooled down efficiently. Asymptotic approximations of the Klein-Nishina regime have been formulated in the last decades in order to account for these corrections in the distribution of particles responsible for the observed spectrum of high energy sources. In this work we presenta a numerical approach of the Klein-Nishina corrections to the radiative cooling. It has been developed to simulate the evolution of a distribution of particles interacting with photons in their surroundings via inverse Compton scattering.

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相对论流出中辐射冷却的数值方法

在耀变体、GRB 或 PWNe 等高能天体物理学场景中，超相对论粒子极有可能通过散射与其环境中的光子相互作用。只要粒子的能量大于相互作用光子的能量，就知道（经典）散射处于汤姆逊状态。否则，量子效应会影响散射截面，我们就会进入所谓的 Klein-Nishina 状态。众所周知，汤姆森体系中的辐射冷却非常有效，可产生软高能谱。然而，观察表明，在许多情况下，某些物体的高能谱是相当困难的。这导致人们认为粒子可能没有被有效冷却。在过去的几十年中，已经制定了 Klein-Nishina 体系的渐近近似，以解释对所观察到的高能源光谱负责的粒子分布的这些修正。在这项工作中，我们提出了对辐射冷却进行 Klein-Nishina 校正的数值方法。它已被开发用于模拟通过逆康普顿散射与周围光子相互作用的粒子分布的演变。