论文标题
在不断发展的超新星残留物中的非平衡离子化和辐射转运
Non-equilibrium ionisation and radiative transport in an evolving supernova remnant
论文作者
论文摘要
We present numerical simulations of the evolution of a supernova (SN) remnant expanding into a uniform background medium with density $n_H = 1.0$ cm$^{-3}$ and temperature of $10^4$ K. We include a dynamically evolving non-equilibrium ionisation (NEI) network (consisting of all the ions of H, He, C, N, O, Ne, Mg, Si, S, Fe),频率依赖性辐射转移（RT），热传导和简单的尘埃演化模型，彼此内部偶联和流体动力学。我们假设球形对称性。取决于局部辐射场和离子分数，计算照片离世，辐射损失，照相，电荷加热/冷却和辐射压力。我们发现，即使在没有非平衡冷却和辐射转运的情况下，也可以通过碰撞平衡冷却曲线对SN残留物的动力学和能量（而不是发射光谱）进行很好的建模。我们发现，在不同阶段，SN残留阶段的前体电离辐射的效果主要取决于电击的快速冷却，并且与稳态冲击不同。与稳态冲击相比，不同离子（例如N II，C IV和N V）的预测色谱柱密度最多可以更高。我们还提供了一些高ES溶解发射光谱，可以将其与观察到的残余物进行比较，以获取有关残留物的物理和化学状态的重要信息，并限制了背景ISM。
We present numerical simulations of the evolution of a supernova (SN) remnant expanding into a uniform background medium with density $n_H = 1.0$ cm$^{-3}$ and temperature of $10^4$ K. We include a dynamically evolving non-equilibrium ionisation (NEI) network (consisting of all the ions of H, He, C, N, O, Ne, Mg, Si, S, Fe), frequency dependent radiation transfer (RT), thermal conduction, and a simple dust evolution model, all intra-coupled to each other and to the hydrodynamics. We assume spherical symmetry. Photo-ionisation, radiation losses, photo-heating, charge-exchange heating/cooling and radiation pressure are calculated on-the-fly depending on the local radiation field and ion fractions. We find that the dynamics and energetics (but not the emission spectra) of the SN remnants can be well modelled by collisional equilibrium cooling curves even in the absence of non-equilibrium cooling and radiative transport. We find that the effect of precursor ionising radiation at different stages of SN remnant are dominated by rapid cooling of the shock and differ from steady state shocks. The predicted column densities of different ions such as N II, C IV and N V, can be higher by up to several orders of magnitude compared to steady state shocks. We also present some high esolution emission spectra that can be compared with the observed remnants to obtain important information about the physical and chemical states of the remnant, as well as constrain the background ISM.
