论文标题
部分可观测时空混沌系统的无模型预测
A Semi-Analytical Line Transfer (SALT) Model III: Galactic Inflows
论文作者
论文摘要
我们介绍了由于气体将光子散射到各向同性发射的辐射来源而导致的紫外光谱的计算。该模型基于Scarlata＆Panagia（2015）的半分析线转移（盐）代码的适应，并旨在解释在部分离子化的银河流入频谱中观察到的逆P-Cygni轮廓。除了介绍该模型外，我们还探讨了流入盐模型的参数空间，并重新创建了各种出于物理动机的场景，包括球形流入，流入的覆盖分数小于统一和银河喷泉（即带有流入和流向成分的银河系系统）。流入气体的结果光谱显示出可能会误解为低分辨率光谱中的ISM功能的光谱特征（$σ\大约120 $ $ \ rm {km} $ $ \ rm \ rm {s}^{ - 1} $），表明带有流动性系统的总数是汇总的。我们的模型表明，中等分辨率的观察（$ r = 6000 $或$σ\大约50美元$ \ rm {km} $ $ \ $ \ rm {s}^{ - 1} $）可以通过800万级望远镜获得，可以解决典型的p cygni periles，以识别出易于识别的特征性倒数。
We present calculations of ultraviolet spectra resulting from the scattering of photons by gas in-falling onto an isotropically emitting source of radiation. The model is based on an adaptation of the semi-analytical line transfer (SALT) code of Scarlata & Panagia (2015), and designed to interpret the inverse P-Cygni profiles observed in the spectra of partially ionized galactic inflows. In addition to presenting the model, we explore the parameter space of the inflowing SALT model and recreate various physically motivated scenarios including spherical inflows, inflows with covering fractions less than unity, and galactic fountains (i.e., galactic systems with both an inflowing and outflowing component). The resulting spectra from inflowing gas show spectral features that could be misinterpreted as ISM features in low resolution spectroscopy ($σ\approx 120$ $\rm{km }$ $\rm{s}^{-1}$), suggesting that the total number of galactic systems with inflows is undercounted. Our models suggest that observations at medium resolution ($R = 6000$ or $σ\approx 50$ $\rm{km }$ $\rm{s}^{-1}$) that can be obtained with 8m-class telescopes will be able to resolve the characteristic inverse P Cygni profiles necessary to identify inflows.
