标题： HD 93129A 的非热辐射模型 显示英文标题

标题： A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A

摘要： 在我们的银河系中，双星系统HD 93129A是已知质量最大的双星之一。 这个系统在射电波段表现出非热辐射，可用于推断其物理条件并预测其在高能波段的辐射。 我们旨在通过建模非热辐射源来限制HD 93129A的一些未知参数，并分析该源在硬X射线和$\gamma$射线中的可探测性。 我们开发了一个宽频谱辐射模型，考虑了沿激波区域加速粒子的演化、不同辐射过程的辐射以及辐射通过局部物质和辐射场时的衰减。 从射电辐射的分析中，我们发现双星HD~93129A更可能具有低倾角和高偏心率。 非热电子的最低能量似乎在$\sim 20 - 100$MeV之间，这取决于风碰撞区域磁场的强度。 后者可能在$\sim 20 - 1500$mG范围内。我们的模型能够再现观测到的射电辐射，并预测HD~93129A的非热辐射将在不久的将来增加。 借助诸如\textit{NuSTAR}、\textit{费米}和CTA的仪器，将能够限制该源的相对论粒子含量以及其他参数，如风碰撞区的磁场强度，从而可以得到大质量恒星表面磁场的上限，进而推断粒子加速区域是否发生了磁场增强。 显示英文摘要

摘要： The binary stellar system HD 93129A is one of the most massive known binaries in our Galaxy. This system presents non-thermal emission in the radio band, which can be used to infer its physical conditions and predict its emission in the high-energy band. We intend to constrain some of the unknown parameters of HD 93129A through modelling the non-thermal emitter, and also to analyse the detectability of this source in hard X-rays and $\gamma$-rays. We develop a broadband radiative model for the wind-collision region taking into account the evolution of the accelerated particles streaming along the shocked region, the emission by different radiative processes, and the attenuation of the emission propagating through the local matter and radiation fields. From the analysis of the radio emission, we find that the binary HD~93129A is more likely to have a low inclination and a high eccentricity. The minimum energy of the non-thermal electrons seems to be between $\sim 20 - 100$MeV, depending on the intensity of the magnetic field in the wind-collision region. The latter can be in the range $\sim 20 - 1500$ mG. Our model is able to reproduce the observed radio emission, and predicts that the non-thermal radiation from HD~93129A will increase in the near future. With instruments such as \textit{NuSTAR}, \textit{Fermi}, and CTA, it will be possible to constrain the relativistic particle content of the source, and other parameters such as the magnetic field strength in the wind collision zone, which in turn can be used to obtain upper-limits of the magnetic field on the surface of the very massive stars, thereby inferring whether magnetic field amplification is taking place in the particle acceleration region.