Grošelj Daniel, Hakobyan Hayk, Beloborodov Andrei M, Sironi Lorenzo, Philippov Alexander
Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, B-3001 Leuven, Belgium.
Department of Astronomy and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA.
Phys Rev Lett. 2024 Feb 23;132(8):085202. doi: 10.1103/PhysRevLett.132.085202.
We report results from the first radiative particle-in-cell simulations of strong Alfvénic turbulence in plasmas of moderate optical depth. The simulations are performed in a local 3D periodic box and self-consistently follow the evolution of radiation as it interacts with a turbulent electron-positron plasma via Compton scattering. We focus on the conditions expected in magnetized coronae of accreting black holes and obtain an emission spectrum consistent with the observed hard state of Cyg X-1. Most of the turbulence power is transferred directly to the photons via bulk Comptonization, shaping the peak of the emission around 100 keV. The rest is released into nonthermal particles, which generate the MeV spectral tail. The method presented here shows promising potential for ab initio modeling of various astrophysical sources and opens a window into a new regime of kinetic plasma turbulence.
我们报告了对中等光学深度等离子体中强阿尔文湍流进行的首次辐射粒子模拟结果。模拟在局部三维周期性盒子中进行，并自洽地跟踪辐射与湍流电子 - 正电子等离子体通过康普顿散射相互作用时的演化。我们关注吸积黑洞磁化日冕中预期的条件，并获得了与观测到的天鹅座X - 1硬态一致的发射光谱。大部分湍流能量通过整体康普顿化直接转移到光子上，形成了约100 keV附近的发射峰值。其余能量释放到非热粒子中，这些粒子产生了兆电子伏特光谱尾部。这里提出的方法在各种天体物理源的从头建模方面显示出有前景的潜力，并为动力学等离子体湍流的新领域打开了一扇窗口。
