论文标题
磁驱动的积聚盘风：气体热力学的作用和与超快速流出的比较
Magnetically driven accretion disc winds: the role of gas thermodynamics and comparison to ultra-fast outflows
论文作者
论文摘要
在发光的活性银河核（AGN）中通常观察到风。这些风的合理模型是磁流失动力学（MHD）圆盘风。如果从薄积聚盘中进行圆盘风，则在此类MHD模型中通常采用等温或绝热假设。在这项工作中，我们进行了二维MHD模拟，以实施不同的热处理（等温，绝热和辐射）来研究它们对薄积聚盘风的影响。我们发现，与通过用辐射冷却和加热来求解能量方程相比，等温模型和绝热模型都高估了温度，低估了温度，无法预测风的局部结构。基于具有辐射冷却和加热的模型，将电离参数，柱密度和圆盘风速度与观察到的超快流出（UFOS）进行了比较。我们发现，在我们的模拟中，不明飞行物只能在数百个Schwarzschild半径内产生。在更大的半径下，找不到不明飞行物。因此，纯MHD风无法解释所有观察到的不明飞行物。
Winds are commonly observed in luminous active galactic nuclei (AGNs). A plausible model of those winds is magnetohydrodynamic (MHD) disc winds. In the case of disc winds from a thin accretion disc, isothermal or adiabatic assumption is usually adopted in such MHD models. In this work we perform two-dimensional MHD simulations implementing different thermal treatments (isothermal, adiabatic and radiative) to study their effects on winds from a thin accretion disc. We find that both the isothermal model and the adiabatic model overestimate the temperature, underestimate the power of disc winds, and cannot predict the local structure of the winds, compared to the results obtained by solving the energy equation with radiative cooling and heating. Based on the model with radiative cooling and heating, the ionization parameter, the column density and the velocity of the disc winds have been compared to the observed ultrafast outflows (UFOs). We find that in our simulations the UFOs can only be produced inside hundreds of Schwarzschild radius. At much larger radii, no UFOs are found. Thus, the pure MHD winds cannot interpret all the observed UFOs.
