论文标题
沿轨道的脉冲星巨星碰撞的动力学和辐射半分析模型：应用于LS 5039
A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039
论文作者
论文摘要
伽马射线二进制文件是在1 meV以上的能量下发出非热辐射的系统。一种建议的场景解释其发射是由旋转巨大恒星的脉冲星组成的，粒子加速发生在恒星和脉冲星风的相互作用中产生的冲击中。我们开发了一个半分析模型的碰撞结构的非热发射，包括轨道运动的动态效应。我们将该模型应用于一般情况，并将模型应用于LS 5039。该模型由一维发射极组成，其几何形状受轨道运动的科里奥利力影响。考虑了两个粒子加速器：一个位于两风向隔离的位置，另一个位于科里奥利力产生的营业额。研究了同步加速器和逆康普顿发射，考虑了与大型恒星相关的多普勒的增强和吸收过程。如果为两个加速器提供相同的能量预算，则大多数辐射都来自科利奥利离职及以后的区域，最多可以从二元系统进行一些轨道分离。该模型使我们能够复制一些LS 5039发射功能，但并非全部。特别是，MEV辐射可能太高，无法单独用我们的模型来解释，而GEV通量已恢复，但没有调制，并且超出Coriolis离职的无线电发射太低。预测的系统倾向与二进制中的脉冲星存在一致。该模型在重现LS 5039的总体非热行为方面非常成功。提出了一些改进来更好地解释该来源中观察到的现象学，例如考虑到粒子再生的粒子重新循环，超出了Coriolis离职，未落后的Pulsar风发射以及发射机的三维扩展。
Gamma-ray binaries are systems that emit non-thermal radiation peaking at energies above 1 MeV. One proposed scenario to explain their emission consists of a pulsar orbiting a massive star, with particle acceleration taking place in shocks produced by the interaction of the stellar and pulsar winds. We develop a semi-analytical model of the non-thermal emission of the colliding-wind structure including the dynamical effects of orbital motion. We apply the model to a general case and to LS 5039. The model consists of a one-dimensional emitter the geometry of which is affected by Coriolis forces owing to orbital motion. Two particle accelerators are considered: one at the two-wind standoff location, and the other one at the turnover produced by the Coriolis force. Synchrotron and inverse Compton emission is studied, accounting for Doppler boosting and absorption processes associated to the massive star. If both accelerators are provided with the same energy budget, most of the radiation comes from the region of the Coriolis turnover and beyond, up to a few orbital separations from the binary system. The model allows us to reproduce some of the LS 5039 emission features, but not all of them. In particular, the MeV radiation is probably too high to be explained by our model alone, the GeV flux is recovered but not its modulation, and the radio emission beyond the Coriolis turnover is too low. The predicted system inclination is consistent with the presence of a pulsar in the binary. The model is quite successful in reproducing the overall non-thermal behavior of LS 5039. Some improvements are suggested to better explain the phenomenology observed in this source, like accounting for particle reacceleration beyond the Coriolis turnover, unshocked pulsar wind emission, and the three-dimensional extension of the emitter.
